uva-dare (digital academic repository) the …...various stages of star formation are represented:...
TRANSCRIPT
UvA-DARE is a service provided by the library of the University of Amsterdam (http://dare.uva.nl)
UvA-DARE (Digital Academic Repository)
The Herschel/HIFI spectral survey of OMC-2 FIR 4 (CHESS). An overview of the 480 to 1902GHz range
Kama, M.; López-Sepulcre, A.; Dominik, C.; Ceccarelli, C.; Fuente, A.; Caux, E.; Higgins, R.;Tielens, A.G.G.M.; Alonso-Albi, T.Published in:Astronomy & Astrophysics
DOI:10.1051/0004-6361/201219431
Link to publication
Citation for published version (APA):Kama, M., López-Sepulcre, A., Dominik, C., Ceccarelli, C., Fuente, A., Caux, E., ... Alonso-Albi, T. (2013). TheHerschel/HIFI spectral survey of OMC-2 FIR 4 (CHESS). An overview of the 480 to 1902 GHz range. Astronomy& Astrophysics, 556, A57. https://doi.org/10.1051/0004-6361/201219431
General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s),other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons).
Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, statingyour reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Askthe Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam,The Netherlands. You will be contacted as soon as possible.
Download date: 08 Feb 2020
A&A 556, A57 (2013)DOI: 10.1051/0004-6361/201219431c© ESO 2013
Astronomy&
Astrophysics
The Herschel/HIFI spectral survey of OMC-2 FIR 4 (CHESS)An overview of the 480 to 1902 GHz range?
M. Kama1,2, A. López-Sepulcre3, C. Dominik2,4, C. Ceccarelli3, A. Fuente5, E. Caux6,7, R. Higgins8,A. G. G. M. Tielens1, and T. Alonso-Albi5
1 Leiden Observatory, PO Box 9513, 2300 RA, Leiden, The Netherlandse-mail: [email protected]
2 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands3 UJF−Grenoble 1/CNRS−INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), UMR 5274, 38041 Grenoble,
France4 Department of Astrophysics/IMAPP, Radboud University Nijmegen, Mailbox 79, Po Box 9010, 6525 AJ, Nijmegen,
The Netherlands5 Observatorio Astronómico Nacional, PO Box 112, 28803 Alcalá de Henares, Madrid, Spain6 Université de Toulouse, UPS−OMP, IRAP, 31400 Toulouse, France7 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France8 KOSMA, I. Physik. Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
Received 17 April 2012 / Accepted 2 May 2013
ABSTRACT
Context. Broadband spectral surveys of protostars offer a rich view of the physical, chemical and dynamical structure and evolutionof star-forming regions. The Herschel Space Observatory opened up the terahertz regime to such surveys, giving access to the funda-mental transitions of many hydrides and to the high-energy transitions of many other species.Aims. A comparative analysis of the chemical inventories and physical processes and properties of protostars of various masses andevolutionary states is the goal of the Herschel CHEmical Surveys of Star forming regions (CHESS) key program. This paper focusseson the intermediate-mass protostar, OMC-2 FIR 4.Methods. We obtained a spectrum of OMC-2 FIR 4 in the 480 to 1902 GHz range with the HIFI spectrometer onboard Herschel andcarried out the reduction, line identification, and a broad analysis of the line profile components, excitation, and cooling.Results. We detect 719 spectral lines from 40 species and isotopologs. The line flux is dominated by CO, H2O, and CH3OH. Theline profiles are complex and vary with species and upper level energy, but clearly contain signatures from quiescent gas, a broadcomponent likely due to an outflow, and a foreground cloud.Conclusions. We find abundant evidence for warm, dense gas, as well as for an outflow in the field of view. Line flux represents 2%of the 7 L� luminosity detected with HIFI in the 480 to 1250 GHz range. Of the total line flux, 60% is from CO, 13% from H2Oand 9% from CH3OH. A comparison with similar HIFI spectra of other sources is set to provide much new insight into star formationregions, a case in point being a difference of two orders of magnitude in the relative contribution of sulphur oxides to the line coolingof Orion KL and OMC-2 FIR 4.
Key words. Astrochemistry – stars: formation – stars: protostars
1. Introduction
With the proliferation of high-sensitivity broadband receivers,wide frequency coverage spectral surveys covering >10 GHzare becoming the norm (e.g. Johansson et al. 1985; Blake et al.1986b; Cernicharo et al. 1996; Schilke et al. 1997; Cernicharoet al. 2000; Caux et al. 2011). Such surveys provide compre-hensive probes of the chemical inventory, excitation conditionsand kinematics of sources such as protostars. Here, we presentthe first Herschel/HIFI spectral survey of an intermediate-massprotostellar core, OMC-2 FIR 4 in the Orion A molecular cloud,covering 480 to 1902 GHz.
The chemical composition of a protostar is linked to its evo-lutionary state and history, for example the relative abundancesof the sulphur-bearing species in a protostellar core depend onthe gas temperature and density, as well as the composition of
? Appendix A is available in electronic form athttp://www.aanda.org
the ices formed during the prestellar core phase (e.g. Wakelamet al. 2005). The chemical makeup of the gas also plays a rolein the physical evolution of the protostar, for example by cou-pling with the magnetic field or by its role in the cooling of thegas (e.g. Goldsmith 2001). The large number of spectral linescaptured by a survey places strong constraints on the excitationconditions and even spatially unresolved physical structure.
The HIFI spectrometer (de Graauw et al. 2010) onboard theHerschel Space Observatory (Pilbratt et al. 2010) made a largepart of the far-infrared or terahertz-frequency regime accessibleto spectral surveys (Bergin et al. 2010; Ceccarelli et al. 2010;Crockett et al. 2010; Zernickel et al. 2012; Neill et al. 2012;van der Wiel et al. 2013). Previous studies at these frequencieshave been mostly limited to small frequency windows on theground or, for space missions such as ISO, orders of magnitudelower spectral resolution and sensitivity than HIFI. Many hy-drides and high-excitation lines of key molecules such as COand H2O are routinely observable while Herschel is operational.
Article published by EDP Sciences A57, page 1 of 36
A&A 556, A57 (2013)
Spectral surveys of star forming regions with HIFI are the focusof the CHESS1 (Ceccarelli et al. 2010) and HEXOS2 (Berginet al. 2010) key programs. A comparison of low- to high-massprotostars, a key goal of CHESS, offers insight into the physicsand chemistry of star formation through the entire stellar massrange. The intermediate-mass protostar in the CHESS sample isOMC-2 FIR 4 in Orion.
Orion is a giant molecular cloud complex at a distanceof ∼420 pc (Menten et al. 2007 found 414 ± 7 pc to the OrionNebula Cluster and Hirota et al. 2007 437± 19 pc to Orion KL).Various stages of star formation are represented: Orion Ia and Ibare 10 Myr old clusters, while Class 0 protostars are still abun-dant in the OMC-1, -2 and -3 subclouds. The OMC-2 cloud corecontains a number of protostars, including OMC-2 FIR 4 as thedominant Class 0 object. It is among the closest intermediate-mass protostellar cores and possibly an example of triggered starformation (Shimajiri et al. 2008).
While earlier studies attributed a luminosity of 400or 1000 L� to OMC-2 FIR 4 (Mezger et al. 1990; Crimieret al. 2009), recent Herschel and SOFIA observations found 30to 50 L� (Adams et al. 2012). Adams et al. (2012) further foundan envelope mass of 10 M� for FIR 4, while previous authorsfound it to be ∼30 M� (Mezger et al. 1990; Crimier et al. 2009)and continuum interferometry has yielded even larger estimates,60 M� (Shimajiri et al. 2008). The factor of 20 difference inluminosity is apparently related to the improved spatial reso-lution of the Herschel and SOFIA data used by Adams et al.(2012) compared to that used in earlier work, as well as to dif-ferences in the SED integration annuli, with one focusing on themid-infrared peak and the other covering the whole millimetresource, as discussed elsewhere (López-Sepulcre et al. 2013b).Our results do not depend on the exact value of the luminosity,although eventually this issue will require a dedicated analysisto facilitate a proper classification of OMC-2 FIR 4.
This paper is structured as follows: the observations, theircalibration and reduction are discussed in Sect. 2; we summarizethe quality and molecular inventory of the data and present arotational diagram analysis in Sect. 3; line profile componentsand energetics are discussed in Sect. 4; and the conclusions aresummarized in Sect. 5.
The reduced data and the list of line detections presented inthis paper will be available on the CHESS key program web-site1. The data can also be downloaded via the Herschel ScienceArchive3.
2. Observations and data reduction
The data, presented in Fig. 1, were obtained with the HIFIspectrometer on the Herschel Space Observatory in 2010 and2011, as part of the Herschel/HIFI guaranteed-time key programCHESS (Ceccarelli et al. 2010). The spectral scan observationswere carried out in dual beam switch (DBS) mode, usingthe Wide Band Spectrometer (WBS) with a native resolutionof 1.1 MHz (0.7 to 0.2 km s−1). The data were downloaded fromthe Herschel Science Archive, re-pipelined, reduced, and thendeconvolved with the HIPE software (Ott 2010, version 6.2.0for the SIS bands and 8.0.1 for the HEB bands). Kelvin-to-Jansky conversions were carried out with the factors given by
1 http://www-laog.obs.ujf-grenoble.fr/heberges/hs3f/;PI Cecilia Ceccarelli.2 http://www.hexos.org; PI Edwin A. Bergin3 http://herschel.esac.esa.int/Science_Archive.shtml
Table 1. Summary of the full-band HIFI observations and of fluxes atselected standard wavelengths.
Band νbanda HPBWb rmsobs
c Lines Fluxd Fνe
GHz ′′ mK GHz−1 W m−2 Jy1a 520 41 16 1.9 5.2(−14) 631b 595 36 16 1.4 7.1(−14) 842a 675 31 30 1.2 1.1(−13) 1062b 757 28 34 1.1 1.3(−13) 1453a 830 26 45 0.7 9.3(−14) 1343b 909 23 40 0.7 2.0(−13) 1564a 1005 21 70 0.7 2.5(−13) 1964b 1084 20 85 0.4 1.7(−13) 2175a 1176 18 158 0.3 3.4(−13) 272158 µm 1902 11 – 153194 µm 1545 14 – 256350 µm 857 25 – 173450 µm 666 32 – 1071a to 5a 1.3(−12)
Notes. (a) The central frequency of the band. (b) Beam size around theband center. (c) rms noise around the band center. (d) Band-integratedflux, in W m−2. The notation is f (g) = f × 10g. Due to overlap betweenthe bands, the sum of band-integrated fluxes exceeds the total at thebottom. (e) Flux at the band center, in Jy.
Roelfsema et al. (2012), which is also the standard reference forother instrumental parameters.
The spectrum on which line identification was carried outwas obtained by stitching together the deconvolved spectralscans and single-setting observations. In case of band overlap,the spectra were cut and stitched at the central frequency of theoverlap. In principle, a lower rms noise could be obtained forthe band overlap regions by combining the data from adjacentbands, but this requires corrections for sideband gain ratio vari-ations, which are still being characterized (see also Sect. 2.3).
2.1. Data quality after reduction
After default pipelining, the data quality is already very high.However, in several bands unflagged spurious features (spurs)prevent the deconvolution algorithm from converging. Thisproblem is resolved by manually flagging the spurs missed bythe pipeline. The baseline level in all bands is mostly gently slop-ing, but has occasional noticeable ripples. The data quality afterspur flagging and baseline subtraction is excellent, as seen inFig. 1. Updated reductions will be provided on the CHESS KPand Herschel Science Center websites.
In bands 1 through 5, an important concern is ghosts frombright (Ta ≥ 3 K) lines (Comito & Schilke 2002). The effect ofghosts on the overall noise properties is negligible, but they maylocally imitate or damage true lines. To check this, we performeda separate reduction where bright lines are masked out and notused in the deconvolution. In bands 6 and 7, we have no ghostproblems, as the signal to noise ratio of even the strongest lines issmall, and ghosts are typically at the scale of double sideband in-tensity variations, which are ≤10% of the peak intensity. Table 1lists the measured root-mean-square (rms) noise for the centralpart of each full band at 1.1 MHz resolution. Bands 6 and 7 wereobserved only partially, their rms noise values can be seen in thebottom panel of Fig. 1.
A57, page 2 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 1. Upper panel: full baseline-subtracted spectral survey (black line) at 1.1 MHz resolution. The set of bright lines towering above the rest isCO, the feature at 1901 GHz is CII. Second panel: full baseline-subtracted spectral survey (black line) on a blown-up y-scale to emphasize weaklines and a second-order polynomial fit (red) to the subtracted continuum in bands 1a through 5a (red). Third panel: Tmb scale integrated intensityof each detected transition. Lower panel: the local rms noise around each detected transition.
A57, page 3 of 36
A&A 556, A57 (2013)
2.2. Line identification
All the lines detected in the survey are summarized in Fig. 1,where we show the full HIFI spectrum, and the integrated fluxand corresponding rms noise level of each line. As the main de-tection criterion, we adopted a limit of S ≥ 5 for the signal tonoise (significance) of the integrated line flux. We use a localdefinition of the signal to noise ratio:
S =
∣∣∣∣∣∣∣∣∫ N
i=1 Tmb,idv
rms · dv ·√
N
∣∣∣∣∣∣∣∣ , (1)
where S is the significance, the integral gives the integrated in-tensity, i is the channel index, Tmb,i is the main beam temperatureof channel i and dv the channel width, N is the number of chan-nels covered by the line, and rms is the local rms noise aroundthe line, measured at a resolution of 1.1 MHz. Given ∼106 chan-nels in the data and a typical extent of 10 . . . 100 channels perline, the total number of false-positives for a flux detection limitof S = 5 in the entire survey is negligible.
Lines in the survey were mostly identified using the JPL4
(Pickett et al. 1998) and CDMS5 (Müller et al. 2005) catalogs.The literature was consulted for H2O+. The line identificationwas carried out in two phases and relied on the fact that theOMC-2 FIR 4 spectrum, while relatively rich in lines, is suffi-ciently sparse at our sensitivity that most lines can be individu-ally and unambiguously identified.
In phase 1, we employed the CASSIS6 software to look fortransitions of more than 80 molecules or isotopologs that hadbeen previously reported in spectral surveys or were expectedto be seen in the HIFI data. Reasonable cutoffs were appliedto limit the number of transitions investigated. For example, forCH3OH, we set Eu < 103 K, Aul > 10−4s−1 and |Ku| ≤ 5, yield-ing >2000 transitions in the HIFI range. The location of each ofthese transitions was then visually inspected in the survey data.Once marked as a potential detection, a feature was not excludedfrom re-examination as a candidate for another species, with theintention of producing a conservative list of blend candidates.For suspected detections, the line flux was measured in a rangecovering the line and accommodating potential weak wings (typ-ically ∼20 km s−1 in total). The local rms noise was determinedfrom two line-free nearby regions for each line, and the line fluxsignal-to-noise ratio was calculated from Eq. (1). The majorityof the investigated transitions were not deemed even candidatedetections, and ∼10% of all chosen candidates turned out to bebelow the S = 5 limit. The identification process was greatlysped up by the use of the CASSIS software as well as customHIPE scripts. Nearly all the lines reported in this paper wereidentified in phase 1.
In phase 2, we performed an unbiased visual inspection ofall the data, looking for features significantly exceeding the lo-cal rms noise level and not yet marked as detections in Phase 1.This process was aided by an automated line-finder that usesa sliding box to identify features exceeding S = 3 and 5 inthe spectral data and also labels all previously identified lines.Phase 2 yielded a large number of candidates, of which only asubset were confirmed as line detections, while the rest failedour signal-to-noise test.
4 http://spec.jpl.nasa.gov/5 http://www.astro.uni-koeln.de/cdms/6 CASSIS has been developed by IRAP-UPS/CNRS,see http://cassis.irap.omp.eu
Fig. 2. Fractional difference of the double-sideband CO line fluxes fromtheir mean for each rotational line. The H polarization is shown inblue (x) and V in red (+). The inset shows the peak line intensity ofthe CO (5−4) transition, highlighted in the main plot with a box, ver-sus intermediate frequency (IF) position. Negative IF frequency denoteslower side band (LSB).
A summary of the detections is given in Sect. 3.1. The bot-tom two panels of Fig. 1 summarize the absolute line fluxes andrms noise values of the detected lines.
2.3. Flux calibration accuracy
For HIFI, instrumental effects such as the sideband gain ratiosand standing waves play a dominant role in the calibration accu-racy and precision (Roelfsema et al. 2012). Standing waves arisefrom internal reflections in the instrument and, to first order, con-tribute a constant .4% to the flux calibration uncertainty acrosseach band. The sideband gain ratio (SBR) characterizes the frac-tion of the total double-sideband intensity that comes from theupper or lower side band (USB, LSB). In an ideal mixer, theUSB and LSB contributions are equal, however in reality thisis not exactly the case, particularly toward the edges of the re-ceiver bands. Here, we discuss the flux calibration uncertainty inthe data, using the overlaps of adjacent HIFI bands, as well as ananalysis of the CO line properties at the double-sideband stage.
Of all the lines in our survey, 10% are in overlapping sectionsof HIFI bands, which we use to obtain a repeat measurement oftheir fluxes after deconvolution, and thus an estimation of thecalibration and processing uncertainties. Focussing on the over-lap of bands 1b and 2a, where the SBR variations are known tobe large (Higgins 2011), we find that the line flux uncertaintyis at the ∼10% level, although this may depend to a substantialdegree on how the data reduction is carried out.
To estimate the SBR impact in the centers of the HIFI bands,we analyze the fluxes of 12CO lines in the double sideband data.In Fig. 2, we show the fractional difference from the mean for theintegrated intensity of each CO line observed in Spectral Scanmode, i.e. with multiple LO settings. H and V polarization areshown in blue (x) and red (+), respectively. The inset in Fig. 2shows the variations of the CO (5−4) line peak intensity with LOsetting, revealing a correlation with the distance of the line fromthe center of the intermediate frequency (IF) range, consistentwith a SBR variation across the band. This correlation is similarfor the other CO lines. There is also a systematic offset between
A57, page 4 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
the intensities in the H and V polarizations, which we do notconsider. We find the relative variations from uncorrected SBRswithin a band to be .4%, although other factors may contributeto the total flux uncertainty budget.
Corrections for the SBR variations are already in the pipelinefor band 2a and are being characterized for all bands (Higginset al. 2009; Higgins 2011). A more thorough analysis of the im-pact of SBRs as well as operations such as baselining and decon-volution on the line fluxes is needed to exploit the full potentialof HIFI. This is particularly important for absorption and weakemission lines.
3. Overview and results
3.1. Detected lines and species
We found and identified a total of 719 lines from 26 molec-ular and atomic species and 14 secondary isotopologs at orabove a flux signal to noise level of 5. All the detected fea-tures were identified, i.e. no unidentified lines remained. Thedetections are summarized in Table 2, and a full list of lines, in-cluding a description of potential blends, is given in Table A.1,in Appendix A. Of the detected lines, 431 or 60% belong toCH3OH. Another 74 or 10% belong to H2CO. In comparison,from SO and SO2 we detect only twelve and two transitions,respectively. Four deuterated isotopologs are detected: HDO,DCN, NH2D and ND. The molecular ions include HCO+, N2H+,CH+, SH+, H2Cl+, OH+ and H2O+.
The upper level energies of the detected transitions rangefrom 24 to 752 K and the typical value is Eu ∼ 100 K, indi-cating that much of the emitting gas in the beam is warm orhot. Many of the transitions have very high critical densities,ncr > 108 cm−3, suggesting that much of the emission originatesin dense gas, probably a compact region. Self-absorption in CO,H2O and NH3 indicates that foreground material is present atthe source velocity, while blueshifted continuum absorption inOH+, CH+, HF and other species points to another foregroundcomponent.
In terms of integrated line intensity, CO dominates with 60%of the total line flux, H2O is second with 13% and CH3OH thirdwith 9%. The line and continuum cooling are discussed in moredetail in Sect. 4.2.
3.2. Line profiles
There is a wealth of information in the line profiles of the de-tected species. Two striking examples are the different line pro-file components revealed by the different molecules and substan-tial changes in line parameters such as vlsr and full-width halfmaximum (FWHM) with changing upper level energy or fre-quency for some molecules.
The statistical significance of the flux of each detected line,by definition, is at least 5σ. For some lines, this makes a vi-sual confirmation unintuitive, however for clarity we preferthe formal signal-to-noise cutoff. As an example, the weakestCS lines are consistent with the intensity as modeled basedon the stronger lines in the rotational ladder. The fluxes inAppendix A originate in channel-by-channel integration, whilethe velocity is given both from the first moment as well as aGaussian fit to the profile, and the FWHM is given only fromGaussian fitting.
The parameters and uncertainties for each transition aregiven in Appendix A. We give here typical uncertainties ofthe Gaussian parameters for the 479 unblended lines. For
vlsr, a cumulative 82% of the lines have uncertainties be-low 0.1 km s−1, 98% fall below 0.5 km s−1 and only one linehas δvlsr > 1 km s−1. This is an H37
2 Cl+ line, which represents aweak set of blended hyperfine components. For FWHM, a cumu-lative 46% of lines have uncertainties below 0.1 km s−1 and 91%are below 0.5 km s−1. Fourteen lines have δFWHM > 1 km s−1,but none of these have FWHM/δFWHM < 5, except for oneweak CH3OH line and the H37
2 Cl+ feature mentioned above.For the purposes of this paper, we distinguish the following
line profile components, as illustrated in Figs. 4 and 3: the qui-escent gas, wings, broad blue, foreground slab, and other. Theirnature is discussed in Sect. 4.1. We emphasize that this is firstand foremost a morphological classification, and that the under-lying spatial source structure may be more complex than is im-mediately apparent from the emergent line profiles.
The quiescent gas refers to relatively narrow lines, FWHM ∼2 . . . 6 km s−1. While it is not clear that 6 km s−1 really orig-inates in quiescent material, currently we lump these veloci-ties together to denote material likely related to various partsof the envelope, to distinguish them from broad lines tracingoutflowing gas. Quiescent gas may have at least two subcom-ponents, one at the source velocity of 11.4 km s−1 and another at12.2 km s−1. The wings refers to a broad component, difficult tofully disentangle but apparently centered around ∼13 km s−1 andwith FWHM ≥ 10 km s−1. The broad blue is traced by SO andis unique for its combination of blueshifted velocity and largelinewidth, both ∼9 km s−1. Other species may have contributionsfrom this component. The foreground slab refers to narrow linesat ∼9 km s−1, most of them in absorption. We use the term otherfor line profile features which do not fall in the above categories.The velocities of all components shift around by ∼1 km s−1 withspecies and excitation energy, pointing to further substructure inthe emitting regions, although part of this variation is certainlydue to measurement uncertainties and could also be due to un-certainties of order 1 MHz in the database frequencies of somespecies.
Using the HIPI7 plugin for HIPE, we inspected severalspecies for contaminating emission in the reference spectra ofthe dual beam switch observations. The species were those withthe strongest lines or where contamination might be suspected.For CO, CI and CII strong emission in one or, in the case of CO,both of the HIFI dual beam switch reference positions createsartificial absorption-like features where emission is subtractedout of the on-source signal. This is evident for CO as deep, nar-row dips in the line profiles, and makes determining the quies-cent gas contribution to these lines very inaccurate. In the caseof CII, the line itself peaks to the blue of the reference positionemission and we judge the problem to be less severe, similarly toCI where only one reference position appears to be substantiallyaffected. The deep self-absorption in several H2O lines appearsto be related to the source. Extended weak H2O 11,0−10,1 emis-sion is present on ∼5′ scales in OMC-2 (Snell et al. 2000), butthis emission seems to peak strongly on OMC-2. Previous obser-vations have demonstrated the large extent of uniform CO 1−0(Shimajiri et al. 2011) and CII emission (Herrmann et al. 1997),consistent with the contamination seen in the HIFI spectra.
3.3. Line density
In Table 1, we give the line density per GHz measured in eachband. The typical value is 1 line GHz−1. At 500 GHz, withrms noise levels of 16 mK, the line density is 1.9 GHz−1, and
7 nhscsci.ipac.caltech.edu/sc/index.php/Hifi/HIPI
A57, page 5 of 36
A&A 556, A57 (2013)
Table 2. Summary of the detected species.
Species # Eu range vlsr FWHM∫
Tmbdv Flux Line componentsK km s−1 km s−1 K km s−1 W m−2
COs1 11 83 . . . 752 11.8 12.3 2.2(3) 2.9(−14) Quiescent gas, wings.13COs2 8 79 . . . 719 11.9 4.7 1.3(2) 1.2(−15) Quiescent gas, wings.C18Os3 5 79 . . . 237 11.3 2.8 1.3(1) 1.1(−16) Quiescent gas.C17Os4 3 81 . . . 151 10.8 3.2 1.6(0) 1.0(−17) Quiescent gas.
H2Os5 11 53 . . . 305 13.1 15.2 4.4(2) 6.2(−15) Quiescent gas, wings.H18
2 Os6 1 61 13.7 19.2 1.1(0) 6.9(−18) Wings.OHs7 6 270 12.7 19.1 8.9(0) 1.9(−16) Wings.OH+ s8 8 44 . . . 50 – – −6.2(0) −7.2(−17) Foreground slab.H2O+ s9 1 54 8.4 2.5 −8.9(−1) −1.2(−17) Foreground slab.
CH3OHs10 431 33 . . . 659 12.2 4.7 5.1(2) 4.5(−15) Quiescent gas.H2COs11 74 97 . . . 732 11.9 4.7 9.5(1) 7.0(−16) Quiescent gas.
HCO+ s12 8 90 . . . 389 11.5 5.4 1.1(2) 9.3(−16) Quiescent gas, wings(?).H13CO+ s12 2 87 . . . 117 11.4 2.2 7.0(−1) 4.4(−18) Quiescent gas.N2H+ s13 7 94 . . . 349 11.7 3.0 2.6(1) 2.2(−16) Quiescent gas.
CIs14 2 24 . . . 63 11.9 1.8 9.6(0) 7.3(−16) Quiescent gas.CIIs15 1 91 9.1 2.1 2.4(1) 5.4(−16) Foreground slab.CH+ s16 1 40 9.8 6.0 −2.8(0) −2.8(−17) Foreground slab.CHs17 3 26 12.7 2.5 4.4(−1) 3.6(−18) Quiescent gas.CCHs18 20 88 . . . 327 – – 1.1(1) 9.0(−17) Quiescent gas, wings.
HCN s19 9 89 . . . 447 12.3 12.1 1.1(2) 9.8(−16)a Quiescent gas, wings.H13CNs20 2 87 . . . 116 12.7 10.0 1.6(0) 1.0(−17) Quiescent gas, wings.HNC s21 2 91 . . . 122 11.6 2.6 2.0(0) 1.3(−17) Quiescent gas.CNs22 20 82 . . . 196 12.5 8.1 1.0(1) 7.5(−17) Quiescent gas, wings.NHs23 5 47 – – –a –a Quiescent gas?NH3
s25 7 28. . . 286 13.3 4.5 2.6(1) 3.2(−16) Quiescent gas, wings.15NH3
s26 1 28 11.3 5.8 1.4(−1) 1.0(−18) Quiescent gas.
CSs27 12 129 . . . 543 12.2 10.3 2.0(1) 1.5(−16) Quiescent gas, wings.C34Ss27 1 127 10.0 1.7 2.1(−1) 1.2(−18) Quiescent gas?H2Ss28 6 55 . . . 103 11.6 5.0 1.4(1) 1.4(−16) Quiescent gas, wings?SOs29 12 166 . . . 321 9.4 9.3 5.5(0) 3.7(−17) Broad blue.SO2
s30 2 65 . . . 379 11.1 10.0 2.7(−1) 1.7(−18) Broad blue, quiescent gas, wings?SH+ s31 2 25 12.6 2.8 2.0(−1) 1.2(−18) Quiescent gas, wings?
HCls32 10 30 . . . 90 11.4 – 4.9(0) 9.8(−17) Quiescent gas, wings.H37Cls32 10 30 . . . 90 11.4 – 9.5(−1) 8.6(−18)b Quiescent gas, wings.H2Cl+ s33 5 23 . . . 58 9.4 1.3 -8.2(−1) 9.3(−18) Foreground slab.H37
2 Cl+ s33 1 58 9.4 1.3 −3.6(−1) −4.4(−18) Foreground slab.
HDOs6 3 43 . . . 95 12.7 3.8 6.5(−1) 6.0(−18) Quiescent gas, wings?DCN s34 2 97 . . . 125 12.0 4.9 3.6(−1) 2.2(−18) Quiescent gas.NDs35 1 25 11.2 2.5 2.6(−1) 1.6(−18) Quiescent gas?NH2Ds36 2 24 11.3 2.6 6.2(−1) 3.6(−18) Quiescent gas.
HFs32 1 59 10.0 2.8 −2.0(0) −2.9(−17) Foreground slab, quiescent gas.Allc 719 23 . . . 752 12.0 5.4 4.0(3) 4.8(−14)
Notes. The table gives the number of detected transitions for each species, the range of upper level energies, the typical vlsr and FWHM, the totalline flux in K km s−1 and in Wm−2, where the exponential is given in brackets, and a note on the dominant line profile components. The line countsinclude hyperfine components and blends. Blends between species are excluded from the per-species flux sums, but included in the total line fluxmeasured in the survey. The species are grouped similarly to Sect. 3.6. Dashes represent cases where a good single Gaussian fit was not obtained,mostly due to blending. (a) NH is unambiguously detected in absorption on the HCN 11 − 10 line.; (b) due to a blend with CH3OH on the 2−1 line,only the H37Cl 1 − 0 flux is given; (c) excluding some blended lines.
References. s1Winnewisser et al. (1997); s2Cazzoli et al. (2004); s3Klapper et al. (2001); s4Klapper et al. (2003); s5Pickett et al. (2005); s6Johns(1985); s7Blake et al. (1986a); s8Müller et al. (2005); s9Mürtz et al. (1998); s10Müller et al. (2004); s11Müller et al. (2000b); s12Lattanzi et al. (2007);s13Pagani et al. (2009); s14Cooksy et al. (1986b); s15Cooksy et al. (1986a); s16Müller (2010); s17McCarthy et al. (2006); s18Padovani et al. (2009);s19Thorwirth et al. (2003); s20Cazzoli & Puzzarini (2005); s21Thorwirth et al. (2000); s22Klisch et al. (1995); s23Flores-Mijangos et al. (2004);s24Müller et al. (1999); s25Yu et al. (2010); s26Huang et al. (2011); s27Kim & Yamamoto (2003); s28Belov (1995); s29Bogey et al. (1997); s30Mülleret al. (2000a); s31Brown & Müller (2009); s32Nolt et al. (1987); s33Araki et al. (2001); s34Brünken et al. (2004); s35Takano et al. (1998); s36Fusinaet al. (1988).
at 1 THz, with rms noise levels of 70 mK, it is 0.7 GHz−1.At 1200 GHz, with and rms noise of 158 mK, the line density
is only 0.3 GHz−1. The frequency resolution is 1.1 MHz inall cases. Clearly, the line density decreases markedly with
A57, page 6 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Table 3. Results of rotational diagram analyses for isotopologs of CO in two upper level energy ranges, Eu < 200 K and Eu > 200 K.
Species Size Eu < 200 K Eu > 200 K Notes
Trot [K] N [cm−2] Trot [K] N [cm−2]
CO beam-filling 208 6.0 × 1016 226 6.6 × 1016 Only wings, |v − vlsr| ≥ 2.5 km s−1.CO beam-filling 67 5.1 × 1017 149 2.4 × 1017 Only wings, optical depth corrected.13CO beam-filling 68 1.3 × 1016 152 4.8 × 1015
C18O beam-filling 52 2.2 × 1015 – –C17O beam-filling 36 1.0 × 1015 – – Two lines (7−6 is excluded).
CO 15” 89 3.4 × 1017 177 2.1 × 1017 Only wings, |v − vlsr| ≥ 2.5 km s−1.CO 15” 45 5.0 × 1018 124 8.7 × 1017 Only wings, optical depth corrected.13CO 15” 46 1.3 × 1017 126 1.8 × 1016
C18O 15” 38 2.3 × 1016 – –C17O 15” 27 1.4 × 1016 – – Two lines (7−6 is excluded).
Notes. Uncertainties for the parameters were calculated including the effects of rms noise and the relative flux calibration errors (10%), and werefound to always be <10%.
frequency. This is due to the decreasing sensitivity of our surveyand the increasing demands on temperature and density to excitehigh-lying rotational levels. A similar decrease for Orion KL wasdiscussed by Crockett et al. (2010). As the line detections coveronly 7% of all frequency channels at 500 GHz, a range wherethe highest number of transitions from CH3OH, SO2 and other“weed” molecules is expected, we conclude that our survey isfar from the line confusion limit.
3.4. The continuum
While continuum emission studies are not the main goal of ourHIFI survey, the high quality of the spectra allows a continuumlevel to be determined for use in line modeling. For example,local wiggles in the baseline can mimick a continuum and dis-tort the absorption line to continuum ratio. We provide here aglobal second-order polynomial fit to the continuum in bands 1athrough 5a, where the data quality is highest and the frequencycoverage is complete. We stitched the spectra with baselines in-tact and sampled every 10th channel to reduce the data volume.All spectral regions containing line detections were excludedfrom the fit. For a polynomial of the formTmb[K] = a + b · ν[GHz] + c · (ν[GHz])2, (2)we find the parameters to be a = − 0.51979, b = 0.0015261and c = −4.1104×10−7. This fit is displayed in the second panelof Fig. 1 and is valid in the range 480 to 1250 GHz.
3.5. Rotational diagrams for CO isotopologs
We performed a basic rotational diagram (Goldsmith & Langer1999) analysis for CO. This is more straightforward than formany other species due to the detection of several isotopologsas well as the low critical density. The results are summarized inTable 3, with rotational excitation temperatures and local ther-modynamic equilibrium (LTE) column densities. The rotationaltemperature, Trot, equals the kinetic one if the emitting mediumis in LTE, and if optical depth effects and the source size areaccounted for. For subthermal excitation, if the source size isknown, Trot gives an upper limit on Tkin, and the obtained col-umn density is a lower limit on the true value. We provide resultsfor two source sizes: beam-filling and 15”. The latter is consis-tent with the dense core (Shimajiri et al. 2008; López-Sepulcreet al. 2013b).
For 12CO, we used only the flux more than 2.5 km s−1 awayfrom the line centre, to avoid the reference contamination thataffects the lower lines. Thus, effectively the 12CO diagram re-sults are for the line wings. In each velocity bin, the 12CO lineswere corrected for optical depth using 13CO, yielding results thatmatch those of 13CO very well. Assuming an isotopolog ratio of63, the 12CO optical depth away from the line centre is foundto be ≤2 and the value decreases with increasing Ju. We expectthe C18O and C17O isotopologs to be optically thin, and a com-parison of their column densities with that of 13CO shows thatthe latter is only slightly optically thick at the line center, whichdominates the flux of this species. For 13CO and C18O, we finda column density ratio of 6, while 7 is expected.
To look for changes with increasing Eu, we perform the anal-ysis in two excitation regimes: Eu < 200 K and Eu > 200 K.We find that Trot increases by a factor of 2−3 with Ju, in otherwords higher-lying transitions have a higher excitation temper-ature. Thus, while the results in Table 3 show that a somewhathigher Trot is found for C18O than for C17O, more lines are de-tected for the former, and fitting the same transitions for bothspecies gives a better match.
Due to its low critical density (n . 106 cm−3 up to Ju = 16),CO is easily thermalized at densities typical of protostellar cores,∼106 cm−3. Such densities may not exist in the regions that emitin the line wings. Therefore, the temperature values in Table 3are upper limits on the kinetic temperature.
Analyses of ground-based observations of C18O inOMC-2 FIR 4 are consistent with our results. The column den-sity we find assuming a beam-filling source, N = 2.2 ×1015 cm−2, is almost exactly the same as that found by Castets& Langer (1995) from the 1−0 and 2−1 lines with with the 15 mSEST telescope, N = 2.5 × 1015 cm−2. Using the IRAM 30 mtelescope and the same transitions, Alonso-Albi et al. (2010)found Trot = 22 K and N = 4.8 × 1015 cm−2. For a centrallyconcentrated source, such an increase of average column densitywith decreasing beam size (θSEST ≈ 2 · θIRAM) is expected, al-though given that the true uncertainties on any column densitydetermination are likely around a factor of two, the differencemay be insignificant. The different C18O rotational temperatures,52 K from HIFI and 22 K from IRAM, again assuming beam-filling, indicate that the high-J lines preferentially probe warmergas, consistent with our rotational diagram results in the low andhigh Eu regimes.
A57, page 7 of 36
A&A 556, A57 (2013)
Fig. 3. Mean velocities and linewidths from Gaussian fits to lines of representative species. Several groups emerge, these are labeled in gray andreferred to in the text. The orange bars give the range of fit parameters of the full set of lines of each species. The black bars, at top left, showthe conservative Gaussian parameter fit uncertainties (see also Sect. 3.2). Where the orange bars are one-sided, showing the conservative fit errors,only a single line was detected or simultaneous fitting of multiple lines forced the species to appear at a single vlsr. For a discussion, see Sect. 4.1.
3.6. Comments on individual species
Here, we comment on each detected species. All quoted line pa-rameters are from single-Gaussian fits, unless explicitly statedotherwise.
3.6.1. CO, 13CO, C18O, C17O
The stitched spectrum of OMC-2 FIR 4 is dominated bythe CO ladder, towering above the other lines in Fig. 1 andshown individually in Fig. 5. The peak Tmb values are in therange 4.4 . . . 20.1 K. The lines are dominated by emission in thewings and quiescent gas velocities, but up to Ju = 11, emis-sion from the reference beams masks the narrower componentand results in fake absorption features due to signal subtraction.With increasing Ju, the Gaussian fit velocity shifts from 11.9to 13.3 km s−1.
As the relative contribution of the wings increases with in-creasing Ju level, or equivalently with decreasing beam size, thewing component likely traces gas that is hotter than any otherimportant CO-emitting region in OMC-2 FIR 4. On the otherhand, referring to the rotational temperatures in Table 3, we seethat the optical depth corrected 12CO wing Trot matches that of
the entire 13CO line very well – there is a correlation betweenthe fluxes in the line wings and centres.
We also detect several lines of the isotopologs 13CO, C18Oand C17O. While C18O and C17O trace the quiescent gas compo-nent, the 13CO lines contain hints of the wings as seen in Fig. 7.From Ju = 5 to 11, the Gaussian linewidth of 13CO increasesnear-linearly from 3 km s−1 to 9 km s−1. With increasing Ju, thewidth of the C18O lines changes from 2 to 3.4 km s−1, a lesspronounced change than 13CO but similar to N2H+.
We list the C17O 6−5 line as blended with CH3OH, but sim-ilar methanol transitions are not detected and the line is un-usually narrow and redshifted to be a CH3OH detection, sug-gesting the flux originates purely in the CO isotopolog. TheC17O 7−6, however, has a significant flux contribution from ablended H2CO line, as evidenced by the detection of formalde-hyde transitions similar to the blended one.
3.6.2. Water: H2O, OH, OH+, H2O+
One of the key molecules observable with HIFI, water, iswell detected in OMC-2 FIR 4, as seen in Figs. 6 and 8.Similarly to CO, the H2O lines are self-absorbed within a∼0.5 km s−1 blueshift from the source velocity, corresponding
A57, page 8 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 4. Main components of the line profiles. The solid vertical lineshows the source velocity, 11.4 km s−1. The two velocity regimes ofquiescent gas are illustrated by C18O and CH3OH. The deep, narrowabsorption feature in CO is due to emission in the reference beams,while the absorption in H2O appears to be source-related. The broadblue component is represented by SO. The HF line traces foregroundmaterial in the foreground slab, at 9 km s−1, with another contributionfrom the quiescent gas.
to the quiescent gas but in absorption. They also clearly dis-play the wings component, Fig. 3 shows the H2O wings arebroader than those of CO and the lines are typically centerednear 13 km s−1. The peak intensity of the lines does not exceed∼4.5 K. The single-Gaussian fit linewidths vary considerably,from 9.9 to 20.5 km s−1, although it must be kept in mind the lineprofiles are complex. The isotopolog H18
2 O, weakly detected, is
Fig. 5. Normalized profiles of the CO lines detected in the survey, dis-played with a vertical offset of unity between each profile. The solidvertical line marks the source velocity of 11.4 km s−1. The wings areincreasingly important toward high rotational levels. Up to Ju = 11,the quiescent gas is masked by contamination in the reference beams,which causes absorption-like dips in the profiles.
centered at vlsr = 13.7 km s−1 and 19.2 km s−1 wide. As seenin the top panel of Fig. 6, the isotopolog profile is flat and weak,
A57, page 9 of 36
A&A 556, A57 (2013)
Fig. 6. Normalized profiles of the H2O lines detected in the survey, dis-played with a vertical offset of 1 between each profile. The solid verticalline marks the source velocity of 11.4 km s−1. The narrow dips are dom-inated by self-absorption.
and thus difficult to interpret, but it appears to be as broad as H2Oitself. The H2O lines point to a complex underlying velocity andexcitation structure within the envelope.
Fig. 7. Normalized line profiles of carbon-bearing species, illustratingtheir different kinematics. The solid vertical line marks the source ve-locity of 11.4 km s−1. The short vertical dashed lines show the CH hy-perfine components except the one the vlsr is centered on. No CASSISmodel was made for CH, see text. The CII absorption at 11 . . . 15 km s−1
is an artefact due to contamination in the reference spectra. The dip inCI at ∼10 km s−1 as also due to reference beam contamination.
The 3/2−1/2 transition of OH, comprizing six hyperfinecomponents, is detected in emission and one set of hyperfinecomponents is shown in Fig. 8. An LTE fit with CASSIS,
A57, page 10 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 8. Normalized line profiles of some oxygen-bearing species, inparticular relating to H2O chemistry. The solid vertical line marks thesource velocity of 11.4 km s−1. The OH, OH+ and H2O+ spectra havebeen gaussian-smoothed to 4 MHz for clarity.
including the hyperfine structure, yields vlsr = 12.7 andFWHM = 19.1 km s−1. This is consistent with the wings com-ponent, of which OH may be the best tracer in terms of lineprofile complexity. The fit is mostly useful for constraining thekinematic parameters of this species – the source size, columndensity and excitation temperature are not well constrained. Inthe best-fit model, the hyperfine components are optically thin(τ . 0.01). The OH line parameters are very similar to thosetypical for H2O and for high-J CO lines.
Multiple OH+ transitions are detected in absorptionat 9.3 km s−1, part of the foreground slab component. We also de-tect the H2O+ 11,1−00,0 line at 8.4 km s−1. Selected lines are pre-sented in Fig. 8. These ions and the tenuous gas they probe areanalyzed in a companion paper (López-Sepulcre et al. 2013a).
3.6.3. CH3OH and H2CO
Lines of CH3OH and H2CO are shown in Fig. 9, although dueto the enormous number of detections the only criterion for thedisplayed subset is to cover upper level energies from ∼100 Kthrough 200 K to 400 K for both species.
CH3OH dominates the number of detected lines inOMC-2 FIR 4 with 431 lines, and H2CO is second with 74.While the median CH3OH velocity is vlsr = 12.2 km s−1 andFWHM = 4.7 km s−1, the lines display a significant trendin vlsr with upper level energy: at Eu = 50 K, they peakat 11.8 km s−1, while by Eu = 450 K, the typical peak hasshifted to 12.5 km s−1. This suggests the low-excitation lines are
Fig. 9. Normalized line profiles of some CH3OH and H2CO lines, rep-resenting, from bottom to top, upper level energies Eu ≈ 100 K, 200 Kand 400 K for both species. The solid vertical line marks the sourcevelocity of 11.4 km s−1.
dominated by the source velocity component of the quiescentgas, while the redshifted (∼12 km s−1) component becomes in-creasingly dominant at high excitation energies. This dominanceof an underlying hot component is in line with the conclusion ofour previous CH3OH analysis (Kama et al. 2010), where a subsetof the lines was presented, including line profiles and rotationaldiagrams.
The H2CO lines range in upper level energy from 97 Kto 732 K, and the median parameters, vlsr = 11.9 km s−1 andFWHM = 4.7 km s−1, are statistically indistinguishable fromthose of CH3OH. The line of sight velocity trend of H2CO alsoresembles that of CH3OH.
As no isotopologs of CH3OH and H2CO are detected andbecause their excitation will be analyzed in a separate paper,we do not give rotational diagram results for these species inTable 3. However, the shifting of the emission peaks with upperlevel energy and frequency suggests these species probe multipleregions of OMC-2 FIR 4.
3.6.4. HCO+ and N2H+
The HCO+ and N2H+ lines, an overview of which can be seenin Fig. 10, are dominated by the quiescent gas component.
A57, page 11 of 36
A&A 556, A57 (2013)
Fig. 10. Selection of normalized line profiles of HCO+ and N2H+, illus-trating trends in the line kinematics. The solid vertical line marks thesource velocity of 11.4 km s−1.
The wings component appears to contribute at a low level toHCO+ emission. Toward higher J levels, the HCO+ lines be-come double-peaked, with one component near 10 km s−1 andanother at 12 km s−1. An examination of Fig. 10 shows that thedouble peak is relevant mostly for the highest HCO+ lines, forwhich the critical densities are ∼108 cm−3 and lower level en-ergies >200 K. The apparent double peak may be due to self-absorption at ∼10 km s−1. There is no indication in the refer-ence spectra of contamination problems for HCO+. H13CO+ is aprime example of the quiescent gas component.
The N2H+ stays single-peaked, but at Eu > 200 K (Ju > 9),the peak redshifts to 12 km s−1. While the N2H+ lines are nar-rower than those of HCO+ by roughly a factor of two, theirwidths and velocities are similar to the H13CO+, C18O andC17O lines.
3.6.5. Carbon: CI, CII, CH, CCH, CH+
Aside from CO, a number of simple carbon-bearing species aredetected. A comparison of some lines of 13CO, CI, CII, CCH,CH and CH+ is given in Fig. 7, indicating substantial variationsin the line profiles.
The CI and 13CO lines also correspond to the quiescent gas.The highest-J 13CO lines show a broad base, likely the wings.The CI lines show an absorption dip at around 10 km s−1, whichis due to emission in the reference positions and may be thecause of the slight redshift observed for CI in Fig. 3. The CI linefluxes from the bulk of OMC-2 FIR 4 are underestimated due tothe self-absorption.
The CII line peaks at 9.5 km s−1 and likely representsemission from the foreground slab. The CII absorption inthe 11 . . . 15 km s−1 velocity range is an artefact caused by emis-sion in the reference position spectra. To estimate the amountof flux lost due to this at the line peak, we reprocessed the datawith one DBS reference spectrum at a time. We established that,while the 11 . . . 15 km s−1 absorption features vary strongly withthe choice of reference spectrum, the 9.5 km s−1 peak variesonly by ∼10%, suggesting that the amount of line flux lost inthis component through reference subtraction is small or that thelarge-scale emission at this velocity around OMC-2 is remark-ably uniform. The latter is unlikely as the difference spectrumof the two reference positions shows a strong positive-negativeresidual, indicating a velocity offset between the components. Ifthe extended CII emission at 9.5 km s−1 in OMC-2 is of com-parable intensity to the detected peak, any intensity fluctuationsmust be at the ≤10% level on a scale of 6′, given a resolutionof 12′′. Accounting for only the upper level population, we ob-tain a lower limit of 3.4 × 1016 cm−2 on the CII column densitytoward FIR 4.
CCH is dominated by the quiescent gas component, butshows evidence for other components. The lines have a broadbase which appears redshifted, perhaps indicating a contributionfrom the wings. The CH lines are slightly redshifted and corre-spond to the quiescent gas emission. No CASSIS model fittingwas done, the line parameters were obtained from a Gaussian fitto a detected isolated hyperfine component. The parameters aresimilar to those of SH+ and HDO. The CH+ ion absorption lineis strongly saturated, leading to the increased linewidth seen inFig. 3, but it is centered on the foreground slab component. Wecompare CH+ and SH+ in Sect. 3.6.7.
3.6.6. Nitrogen-bearing molecules
Aside form N2H+, which is covered in Sect. 3.6.4, the main de-tected nitrogen-bearing species are HCN, CN, HNC and the ni-trogen hydrides. There are substantial differences in the profileswith species as well as with upper level energy for the nitrogen-bearing species, similarly to carbon and sulphur. In Fig. 11, linesof several representative nitrogen-bearing molecules are shownon a common velocity scale.
HCN, CN and HNC. Gaussian fits to the HCN lines peakat 12.1 km s−1. Their large linewidth, characteristic of the wingscomponent, puts them close to CO and H2O in Fig. 3. Theupper level energies of the detected HCN lines range from 89to 447 K. The high-lying lines, in particular, have critical den-sities around 1010 cm−3, indicating that the emitting regionscontain very dense and hot gas. The H13CN profiles are alsobroad, although they show a peak corresponding to the quies-cent gas.
A57, page 12 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 11. Examples of normalized line profiles of nitrogen-bearingspecies. The solid vertical line marks the source velocity of 11.4 km s−1.The top line profile is centered on HCN and the dashed vertical linesmark the locations of the strongest NH hyperfine components.
The two detected HNC lines trace the quiescent gas compo-nent. The CN line profiles are dominated by the quiescent gascomponent, but there is also a contribution from the wings, asseen in Fig. 11.
NH and NH3. We detect some hyperfine components of theNH 12−01 transition in absorption on the HCN 11−10 emis-sion line, as shown in Fig. 11. The lines are close to the qui-escent gas component velocity. The dominant hyperfine com-ponents are in absorption until below the continuum level. TheND (12,3,4−01,2,3) transition is detected in emission and is shownin Fig. 14.
Seven transitions of NH3 are detected, covering 28 through286 K in upper level energy. As seen in Fig. 11, the lines have
Fig. 12. Examples of normalized line profiles of sulphur-bearingspecies. The solid vertical line marks the source velocity of 11.4 km s−1.The CASSIS model for SH+, showing two hyperfine components, isgiven by the dashed red line.
a broad base, consistent with the wings, and they show narrowself-absorption near the quiescent gas component. We find noevidence for emission in the reference positions to be causingthe absorption, but due to the relative weakness of the featuresthis cannot be fully excluded at present. While the lines havea similar appearance to CO, H2O and OH, and are centeredat the same velocity, they are typically a factor of four nar-rower, as seen in Fig. 3. We return to this point in Sect. 4.1.The fundamental ortho-NH3 line has a particularly interest-ing profile, with a sharp peak at 12.5 km s−1 and a plateauat 10 . . . 12 km s−1.
A57, page 13 of 36
A&A 556, A57 (2013)
3.6.7. Sulphur-bearing molecules
The detected sulphur-bearing species are CS, C34S, H2S, SO,SO2 and SH+. As seen from the selection of lines in Fig. 12,there are significant differences between their line profiles.
The detected CS lines cover an upper level energy range of129 K ≤ Eu ≤ 543 K and seem similar to CO in that they mayhave contributions from the quiescent gas and the wings. Thecritical densities of the high-lying lines are n > 108 cm−3, indi-cating the presence of dense and hot gas in the emitting regions.The C34S 10−9 line is narrow and peaks at around 10 km s−1,likely tracing a dense, warm clump with a high CS abundance, atthat velocity. The clumpy distribution of C34S in OMC-2 FIR 4is explored further by López-Sepulcre et al. (2013b).
The H2S lines are dominated by the quiescent gas compo-nent, but the wings or broad blue components may be present ata low level.
The SO lines are the sole clear tracer of the broad blue com-ponent. They cover an upper level energy range of 165 to 321 Kand have critical densities of order 108 cm−3, suggesting denseand hot gas in the emission region. It is notable that the SO linesare 9.3 km s−1 broad and peak at 9.4 km s−1, 2 km s−1 to the bluefrom the OMC-2 systemic velocity. We detect only two transi-tions of SO2, which are similar in their median properties to CO,perhaps having contributions from the broad blue, quiescent gasand wings components.
The detected SH+ hyperfine line emission is shown in thelowest part of Fig. 12. The line profiles are very similar to CH,as seen in Fig. 3 and by comparing with the second-to-lowestpanel in Fig. 7. The line parameters were obtained by fitting thehyperfine structure with the CASSIS software, and found to bevlsr = (12.6 ± 0.3) km s−1 and FWHM = (2.8 ± 0.3) km s−1.The central velocity of SH+ matches that of the wings compo-nent, but the linewidth resembles the quiescent gas. It is inter-esting to note that we detect CH+ in absorption at 9.8 km s−1
and SH+ in emission around 12.2 km s−1, contrary to the strongcorrelation between these species seen in a sample of galacticsight-lines by Godard et al. (2012). The synthesis path of SH+
is S+ + H2 → SH+ + H, which has an activation barrierof 9860 K, more than twice the 4640 K barrier to the productionof CH+ via an analogous path. This may offer an explanation toour nondetection of SH+ in the foreground slab component, butit is not immediately clear why we do not detect CH+ at the samevelocity as SH+ – excitation and chemistry may both play a role.In the models of Bruderer et al. (2010), there are regions near aprotostellar outflow base where the SH+ abundance is elevatedby several orders of magnitude with respect to that of CH+ dueto sulphur evaporation from grains.
3.6.8. Chlorine-bearing molecules
Lines of isotopologs containing 35Cl and 37Cl of two of themain chlorine-bearing molecules are detected: HCl 1−0 and2−1, and H2Cl+ 1−0 and 2−1. For HCl, the line peak is at∼11.4 km s−1, the quiescent gas velocity. There is a broadbase which may be identified with the wings component. ForH2Cl+, we fitted the hyperfine structure with CASSIS, obtainingvlsr = (9.4 ± 0.2) km s−1 and FWHM = (1.8 ± 0.5) km s−1.Several examples of transitions of chlorine-bearing species areshown in Fig. 13.
Hydrogen chloride is predicted to be the dominant gas-phase chlorine reservoir in high-extinction regions (Blake et al.1986b; Neufeld & Wolfire 2009), consistent with the expectationthat the 11.4 km s−1 component traces the large-scale envelope.
Fig. 13. Normalized line profiles of the main detected HCl andH2Cl+ transitions. The solid vertical line marks the source velocity of11.4 km s−1. The CASSIS models for each species, used to obtain thevlsr and width of the lines, are shown with red dashed lines.
On the other hand, H2Cl+ is predicted to be a significant car-rier in photon-dominated regions, and correspondingly H2Cl+ isdetected in absorption in the blue-shifted foreground slab com-ponent. The chlorine-bearing species will be the focus of an up-coming paper (Kama et al., in prep.).
3.6.9. Deuterated species
Our HIFI survey is poor in deuterated species, the only de-tections are HDO, DCN, NH2D and ND. The strongest linesare shown in Fig. 14. The HDO lines are very weak, there-fore firm conclusions cannot be drawn, but the 11,1−00,0 lineshown in Fig. 14 suggests similarities with H18
2 O in velocity,and our tests with Gaussian decomposition of the H2O linesalso suggest a similar emission peak location. The DCN me-dian vlsr is 12 km s−1, consistent within the errors with HCN butwith the linewidth again much narrower and corresponds to theredshifted side of the quiescent gas component, also traced byCH3OH and H2CO. Singly deuterated ammonia, NH2D, peaksat vlsr ≈ 11.2 km s−1 and corresponds well to other tracers of thequiescent gas component. The ND line is centered near the qui-escent gas velocity but its width corresponds better to the wingsor broad blue component. However, the line is weak and shouldbe interpreted with caution.
3.6.10. HF
The J = 1−0 transition of hydrogen fluoride is detected in ab-sorption at 10.0 km s−1, and is shown in Fig. 4. The linewidthis 2.8 km s−1 and the estimated column density (1.2 ± 0.3) ×1013 cm−2. Modeling by López-Sepulcre et al. (2013a) sug-gests the presence of two different velocity components: one at9 km s−1, corresponding to the foreground slab, and a dominantcomponent around 11 km s−1, roughly the quiescent gas velocity.
A57, page 14 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 14. Selection of lines of deuterated species. A water line has beenadded for comparison with HDO. The solid vertical line marks thesource velocity of 11.4 km s−1. The CASSIS model for ND is markedwith a dashed red line.
4. Discussion
Much information about the kinematic, excitation and abun-dance structure of OMC-2 FIR 4 is encoded into the roughly700 detected spectral lines. The source is kinematically andchemically complex. Substantial amounts of molecular gas arepresent in the HIFI beam at all probed scales (40′′. . . 11′′or 17 000 AU. . . 5000 AU). We detect emission from high-J tran-sitions of CO, CS, HCN, HCO+ and other species. The high crit-ical densities (up to n ∼ 109 cm−3) and excitation energies indi-cate that at least some of the emitting regions are very dense andhot or able to excite some transitions via infrared pumping. Wefocus below on the kinematical components and the energetics,deferring more detailed analyses to future papers.
4.1. Interpretation of the kinematic components
We now discuss the characteristics and possible nature of thekinematic components defined in Sect. 3.2. We emphasize againthat the features discussed are predominantly line profile com-ponents and need not have a one-to-one correspondonence withactual source components. The diversity of line profile shapes is,in any case, a clear indication of the complexity of the underly-ing spatial variations of composition, density, temperature andvelocity.
A correlation between the rotational temperature of the12CO line wings and entire 13CO lines was pointed out inSect. 3.6.1. This is based on a 12CO flux integration starting from±2.5 km s−1 from the line centre, and it is not clear if the sameresult would be found if the integration only included emissionfrom much higher velocities, e.g. starting from ±10 km s−1. If thecorrelation holds, it implies that there is a physical connectionbetween the emission in the CO line centre and high-velocitywings and a Gaussian decomposition into a narrow and broadcomponent may not be useful. This may contribute to a betterunderstanding of the origin of the CO emission. The results of adetailed study of the CO and H2O line wings will be presented ina separate paper (Kama et al., in prep.). For the moment, we pro-ceed with describing the morphological components proposedearlier in this paper.
Quiescent gas. This line profile component may have sev-eral subcomponents. One, centered around 11.0 . . . 11.5 km s−1,likely corresponds to the large-scale (∼104 AU or 25′′) envelopeof OMC-2 FIR 4 and matches the velocity of the bulk OMC-2cloud (Castets & Langer 1995; Aso et al. 2000). This componentis most clearly seen in C18O, C17O, N2H+ and NH2D, and it ap-pears to contribute to the emission of most detected species. Theother component is centered near 12.2 km s−1 and is best tracedby CH3OH, H2CO and DCN. We reiterate that some of the linesclassified as quiescent gas have substantial widths, >5 km s−1,however we lump them together with other lines which are rela-tively narrow when compared to the broadest lines, which musttrace outflowing rather than envelope material.
The H2O, NH3 and high-J HCO+ self-absorption (if HCO+
is indeed self-absorbed) is blueshifted with respect to the sourcerest frame. One hypothesis for explaining this blueshifted self-absorption feature is a slowly expanding layer of warm gas in theinner envelope. Similar absorption features on broad H2O lineprofiles in a sample of protostars are discussed as originating inthe inner envelope by Kristensen et al. (2012), who successfullyreproduced such line profiles with an adaptation of the Myerset al. (1996) model, incorporating outflow emission partially ob-scured by an expanding layer of less excited gas.
Our previous analysis of CH3OH lines in a subset of thepresent data revealed that the quiescent gas component is domi-nated at high upper level energies by a compact, hot component,which we identified with a hot core (Kama et al. 2010). The rota-tional diagram results for other species in Table 3 provide furtherevidence for the importance of an underlying hot component.
Wings. The broad wings are seen most clearly in OH, H2Oand CO, and likely trace at least one outflow. The existence ofa broad component in the CO 3−2 line was noted already byJohnstone et al. (2003). An interpretation of this component ismade difficult by the projected overlap of OMC-2 FIR 4 and onelobe of an outflow from the nearby source, FIR 3 (Shimajiri et al.2008). Given the prominence and symmetry of the wings in thehigh rotational lines of CO, and the broadness of the HCN andCS lines – all indicative hot or dense emitting material – the wing
A57, page 15 of 36
A&A 556, A57 (2013)
emission may originate in a compact outflow from FIR 4 itself(Kama et al., in prep.).
Broad lines of OH correlate well with water and are as-sociated with outflow shocks (Wampfler et al. 2010) and inOMC-2 FIR 4, the large width of the OH lines (FWHM =19.1 km s−1) is consistent with an outflow shock origin.Furthermore, our modeling finds the OH lines to be opticallythin, so together with the highest-J CO lines, OH may be themost straightforward tracer of this outflow.
In Fig. 3, NH3 corresponds to the outflow tracers CO, H2Oand OH in terms of vlsr, but has a typical linewidth a factor offour smaller. In the L1157-B1 outflow context, similar observa-tions have been explained with a model where NH3 is destroyedin a shock at velocities >15 km s−1, while H2O, for example,maintains its high abundance (Viti et al. 2011). Other species,such as CH3OH and H2CO, should also show emission at theoutflow velocity, and a weak wing seems to indeed be present.
Broad blue. This component only appears clearly in linesof SO, although other species such as CO and CS do have ablue wing component that may be related. Its nature is unclear.It may be related to the compact blueshifted spot seen in low-frequency interferometry of SiO and other species by Shimajiriet al. (2008). Indeed, the SiO lines in our follow-up survey withthe IRAM 30 m telescope also show a blueshifted emissioncomponent.
Foreground slab. The slab component, at vlsr ∼ 9.5 km s−1,is traced almost exclusively by absorption lines of molecularions associated with photon-dominated regions (PDRs), suchas OH+, H2O+ and H2Cl+. The CII emission peak also corre-sponds to this component, as does part of the absorption in thefundamental line of HF. In addition to the set of species trac-ing the component, the fact that absorption is seen in low-lyinglines suggests a very tenuous medium. In a companion paper(López-Sepulcre et al. 2013a), we present a detailed analysis ofthis component, finding it to be a low-density and low-extinction(Av ≈ 1 mag) PDR cloud in front of OMC-2, irradiated on oneside by a heavily enhanced FUV field.
Other. Aside from the above four components, there is vari-ation in line profiles between different species, upper level en-ergies and observing frequencies. This includes the evolution ofN2H+ and especially HCO+ line profiles with increasing J level(Fig. 10) and the plateau-and-peak profile of the fundamentalortho-NH3 line (Fig. 11). Many of these line profile aspectsmay be subcomponents of the quiescent gas and other afore-mentioned categories. A full interpretation of this variety of fea-tures, while important, is outside the scope of this paper. Pendingfurther analyses of the HIFI data, we refer the reader to pre-vious (Shimajiri et al. 2008) and upcoming (López-Sepulcreet al. 2013b) papers for interferometric results on the small-scalestructure of OMC-2 FIR 4.
4.2. Line and continuum cooling
We investigated the role of molecular line emission in gas cool-ing by summing the integrated intensities of the detected transi-tions of each species. The results are given in the second-to-lastcolumn of Table 2, and in Fig. 15, we show the 11 dominantcooling molecules. Within the frequency coverage of the survey,CO is the dominant molecular coolant, emitting 60% of the totalenergy in the detected lines. The second most important is H2Owith 13% and the third is CH3OH with 9%. Two other notablecoolants are HCO+ and HCN, both contributing 2% of the totalline flux.
Fig. 15. Fractional contribution of various species to the line emissionfrom OMC-2 FIR 4. The 11 dominant cooling species, integrated acrossthe entire 480 to 1902 GHz HIFI survey, are displayed. Note that theunits are in percent of the total line flux in the HIFI survey, excludingcontinuum emission.
Due to contamination in the reference positions, the total fluxin CO lines is likely underestimated by a few tens of percent, asestimated from the lack of contamination in Ju > 11 and amulticomponent analysis of the lower-J lines. Thus, the true COto total line flux ratio may be as high as ∼70 . . . 80%.
To measure the relative importance of line and contin-uum cooling, we integrated the spectra with baselines intactin the fully frequency sampled region of the survey (bands 1athrough 5a or 480 to 1250 GHz), obtaining a flux of 1.3 ×10−12 W × m−2. Of this, 2.7 × 10−14 W × m−2 or 2% is inlines. In their 300 GHz range study of five low- to intermediate-luminosity protostars including OMC-2 FIR 4, Johnstone et al.(2003) found lines to contribute <8% of the measured contin-uum in their entire sample, consistent with our terahertz-rangeresult. Assuming a distance of 420 pc, the flux we measure withHIFI between 480 and 1250 GHz corresponds to a luminosity of∼7 L�, of which 0.1 L� is line emission.
It is remarkable that the sulphur oxides, SO and SO2, con-tribute negligibly to the line cooling in OMC-2 FIR 4, in strikingcontrast to Orion KL, as discussed in Sect. 4.2.1.
As the frequency coverage above 1250 GHz is not complete,the cooling contributions of some species in the HIFI range maydiffer from those given in Table 2, but for most species the to-tal line fluxes should not differ much from their total 480 to1902 GHz fluxes. Undetected weak lines contributing to the con-tinuum may also introduce a small correction to the quoted num-bers. The total line emission from OMC-2 FIR 4 may have alarge contribution from CO, H2O and OI lines outside the highend of the HIFI frequency range, toward the mid- and near-infrared. A study of the spectrally unresolved CO lines seen to-ward OMC-2 FIR 4 with Herschel/PACS by Manoj et al. (2013)determined the CO luminosity between Ju = 14 and 46 to be0.3 L�. A comparison of this with our HIFI CO line luminosityof 0.1 L� shows that transitions at frequencies within the HIFIrange contribute roughly the same total flux as those at higherfrequencies. As the HIFI and PACS ranges overlap, the total COluminosity from this region cannot be much above 0.4 , which isbetween 0.04% and 0.8% of the total luminosity, depending onthe source luminosity estimate (50 to 1000 L�, as discussed inSect. 1).
A57, page 16 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Fig. 16. Line cooling in the 795−903 GHz range in two sources inOrion. The symbols mark the percentage of line emission in each dom-inant cooling species in OMC-2 FIR 4 (crosses, this work) and inOrion KL (circles, Comito et al. 2005). The upper limits are 5σ. Notethat the units are in percent of all line flux within the 795 to 903 GHzrange, excluding continuum emission.
4.2.1. Comparison with other sources
As a detailed comparison with other sources is outside the scopeof this paper, we provide here an initial view.
In Fig. 16, we compare the relative line cooling in the 795through 903 GHz range in OMC-2 FIR 4 and Orion KL, a well-studied strong line and continuum emitter. The numbers hereare not to be confused with the results for the entire surveygiven above, furthermore the units here are K km s−1, while thefull-survey fluxes were compared on the W m−2 scale. The se-lected species contain the seven most important coolants for ei-ther source. H2O is not considered in this comparison as it hasno lines in the 795 to 903 GHz range. In OMC-2 FIR 4 in thisrange, CO emission contains 61% of the line energy, followedby CH3OH with 20%, HCN with 8% and HCO+ with 7%. InOrion KL, SO2 dominates with 24% of the energy, followed byCH3OH with 22%, CO with 16% and SO with 12%.
While the sulphur oxides contribute at the 10 . . . 20% levelto line cooling in Orion KL, in OMC-2 FIR 4 both con-tribute ≤0.1% in the 795 to 903 GHz range, a difference of atleast two orders of magnitude. This may be due to an excep-tional contribution of energetic shocks in Orion KL. A simi-lar scarcity of sulphur oxides in comparison to Orion KL hasbeen reported before in samples of low- as well as high-massprotostars (Johnstone et al. 2003; Schilke et al. 2006). In addi-tion to shocks, factors such as the thermal evolution of the gasand dust may also play an important role in abundance varia-tions of sulphur-bearing molecules (Wakelam et al. 2004, 2005).The difference of peak velocity we observe between SO andCH3OH, ∼2 km s−1, suggests that SO emission in OMC-2 FIR 4is dominated by a spatially distinct region, a result seen also inSagittarius B2 (Nummelin et al. 2000).
The nature and heating processes of Orion KL are currentlyunder debate in the community and our comparison once againconfirms the exceptional nature of this source. It must be keptin mind that the quoted Orion KL observations were carriedout with the Caltech Submillimeter Observatory, with a beamroughly a third the size of that of Herschel at equivalent fre-quencies, therefore beam dilution effects may be important and
the above comparison should be repeated with the HIFI sur-vey of that source (Crockett et al., in prep.). The acceleratingpublication of HIFI spectral surveys and line observations ofa number of other protostars (e.g. Zernickel et al. 2012; Neillet al. 2012; Caux et al., in prep., see also other papers fromthe CHESS, HEXOS, and WISH key programs) will soon al-low more, and more detailed, comparative analyses to be made,across molecular species as well as protostellar properties. Forexample, the number of species found in the HIFI spectral sur-vey of OMC-2 FIR 4, 26 excluding isotopologs, is smallerthan that found in similar data for the high-mass star form-ing regions NGC 6334I (46 species, Zernickel et al. 2012) andSagittarius B2(N) (≥40 species, Neill et al. 2012). This may berelated to the substantially lower luminosity of OMC-2 FIR 4compared to the more massive sources.
5. Conclusions
– We present a Herschel/HIFI spectral survey of OMC-2 FIR 4in the range 480 to 1901 GHz, one of the first spectral sur-veys of a protostar in the terahertz regime.
– We find 719 lines in the survey, originating from 26 differentmolecular and atomic species and tracing a large range ofexcitation conditions, with 24 ≤ Eu ≤ 752 K.
– The line profiles have contributions from the large-scale en-velope of OMC-2 FIR 4, at least one outflow, a newly dis-covered foreground PDR and other components. The broadoutflow emission has a redshifted offset of 1.5 km s−1 fromthe source velocity. Narrow, blue-shifted self-absorption onbroad emission lines of H2O, NH3, and possibly HCO+,may originate in an expanding layer in the inner envelope.Broad, blue-shifted SO lines trace a new component of un-clear nature.
– The cooling budget of OMC-2 FIR 4 between 480 and1250 GHz is dominated by continuum radiation, with linescontributing 2%. The total flux received in this range is1.3 × 10−12 Wm−2 or ∼7 L� at 420 pc.
– Of all the detected line flux in W×m−2, 60% is from 12CO,13% from H2O and 9% from CH3OH. Every other speciescontributes at the ≤2% level.
– The dominant cooling molecules in OMC-2 FIR 4 andOrion KL are similar, but the relative role of SO and SO2in the energy budget of OMC-2 FIR 4 is two orders of mag-nitude smaller than in Orion KL, indicating a substantial dif-ference in the role of shocks or in the thermal evolution.
– In terms of composition and dominant chemical species,OMC-2 FIR 4 is well in line with results for other pro-tostars from ground-based instruments. It is thus a nearbyintermediate-mass star formation laboratory for which an ex-ceptional spectral dataset is now available.
Acknowledgements. The authors would like to thank Charlotte Vastel for helpwith the spectroscopic data; our CHESS, HEXOS and WISH colleagues for use-ful discussions; and the HIFI Instrument Control Center and Herschel ScienceCenter teams for their efforts. M.K. gratefully acknowledges funding from theNetherlands Organisation for Scientific Research (NWO) Toptalent grant num-ber 021.002.081, the Leids Kerkhoven-Bosscha Fonds and the COST Actionon Astrochemistry. A.L.S. and C.C. acknowledge funding by the French SpaceAgency CNES and from ANR contract ANR-08-BLAN-022. A.F. acknowledgessupport from the CONSOLIDER INGENIO 2010 program, grant CSD2009-00038. Herschel is an ESA space observatory with science instruments providedby European-led Principal Investigator consortia and with important participa-tion from NASA. This work is based on analysis carried out with the CASSISsoftware, developed by IRAP-UPS/CNRS (http://cassis.irap.omp.eu).
A57, page 17 of 36
A&A 556, A57 (2013)
References
Adams, J. D., Herter, T. L., Osorio, M., et al. 2012, ApJ, 749, L24Alonso-Albi, T., Fuente, A., Crimier, N., et al. 2010, A&A, 518, A52Araki, M., Furuya, T., & Saito, S. 2001, J. Mol. Spectr., 210, 132Aso, Y., Tatematsu, K., Sekimoto, Y., et al. 2000, ApJS, 131, 465Belov, S. 1995, J. Mol. Spectr., 173, 380Bergin, E. A., Phillips, T. G., Comito, C., et al. 2010, A&A, 521, L20Blake, G. A., Farhoomand, J., & Pickett, H. M. 1986a, J. Mol. Spectr., 115, 226Blake, G. A., Masson, C. R., Phillips, T. G., & Sutton, E. C. 1986b, ApJS, 60,
357Bogey, M., Civiš, S., Delcroix, B., et al. 1997, J. Mol. Spectr., 182, 85Brown, J. M., & Müller, H. S. P. 2009, J. Mol. Spectr., 255, 68Bruderer, S., Benz, A. O., Stäuber, P., & Doty, S. D. 2010, ApJ, 720, 1432Brünken, S., Fuchs, U., Lewen, F., et al. 2004, J. Mol. Spectr., 225, 152Castets, A., & Langer, W. D. 1995, A&A, 294, 835Caux, E., Kahane, C., Castets, A., et al. 2011, A&A, 532, A23Cazzoli, G., & Puzzarini, C. 2005, J. Mol. Spectr., 233, 280Cazzoli, G., Puzzarini, C., & Lapinov, A. V. 2004, ApJ, 611, 615Ceccarelli, C., Bacmann, A., Boogert, A., et al. 2010, A&A, 521, L22Cernicharo, J., Barlow, M. J., Gonzalez-Alfonso, E., et al. 1996, A&A, 315,
L201Cernicharo, J., Guélin, M., & Kahane, C. 2000, A&AS, 142, 181Comito, C., & Schilke, P. 2002, A&A, 395, 357Comito, C., Schilke, P., Phillips, T. G., et al. 2005, ApJS, 156, 127Cooksy, A. L., Blake, G. A., & Saykally, R. J. 1986a, ApJ, 305, L89Cooksy, A. L., Saykally, R. J., Brown, J. M., & Evenson, K. M. 1986b, ApJ,
309, 828Crimier, N., Ceccarelli, C., Lefloch, B., & Faure, A. 2009, A&A, 506, 1229Crockett, N. R., Bergin, E. A., Wang, S., et al. 2010, A&A, 521, L21de Graauw, T., Helmich, F. P., Phillips, T. G., et al. 2010, A&A, 518, L6Flores-Mijangos, J., Brown, J. M., Matsushima, F., et al. 2004, J. Mol. Spectr.,
225, 189Fusina, L., di Lonardo, G., Johns, J. W. C., & Halonen, L. 1988, J. Mol. Spectr.,
127, 240Godard, B., Falgarone, E., Gerin, M., et al. 2012, A&A, 540, A87Goldsmith, P. F. 2001, ApJ, 557, 736Goldsmith, P. F., & Langer, W. D. 1999, ApJ, 517, 209Herrmann, F., Madden, S. C., Nikola, T., et al. 1997, ApJ, 481, 343Higgins, R. 2011, Ph.D. Thesis, NUI MaynoothHiggins, R. D., Pearson, J. C., Lord, S. D., & Teyssier, D. 2009, in 64th
International Symposium On Molecular SpectroscopyHirota, T., Bushimata, T., Choi, Y. K., et al. 2007, PASJ, 59, 897Huang, X., Schwenke, D. W., & Lee, T. J. 2011, J. Chem. Phys., 134, 4321Johansson, L. E. B., Andersson, C., Elder, J., et al. 1985, A&AS, 60, 135Johns, J. W. C. 1985, J. Opt. Soc. Am. B Opt. Phys., 2, 1340Johnstone, D., Boonman, A. M. S., & van Dishoeck, E. F. 2003, A&A, 412, 157Kama, M., Dominik, C., Maret, S., et al. 2010, A&A, 521, L39Kim, E., & Yamamoto, S. 2003, J. Mol. Spectr., 219, 296Klapper, G., Lewen, F., Gendriesch, R., Belov, S. P., & Winnewisser, G. 2001,
Z. Naturforschung Teil A, 56, 329Klapper, G., Surin, L., Lewen, F., et al. 2003, ApJ, 582, 262Klisch, E., Klaus, T., Belov, S. P., Winnewisser, G., & Herbst, E. 1995, A&A,
304, L5Kristensen, L. E., van Dishoeck, E. F., Bergin, E. A., et al. 2012, A&A, 542, A8Lattanzi, V., Walters, A., Drouin, B. J., & Pearson, J. C. 2007, ApJ, 662, 771López-Sepulcre, A., Kama, M., Ceccarelli, C., et al. 2013a, A&A, 549, A114
López-Sepulcre, A., Taquet, V., Sánchez-Monge, Á., et al. 2013b, A&A, in press,DOI: 10.1051/0004-6361/201220905
Manoj, P., Watson, D. M., Neufeld, D. A., et al. 2013, ApJ, 763, 83McCarthy, M. C., Mohamed, S., Brown, J. M., & Thaddeus, P. 2006, Proc. Nat.
Acad. Sci., 103, 12263Menten, K. M., Reid, M. J., Forbrich, J., & Brunthaler, A. 2007, A&A, 474, 515Mezger, P. G., Zylka, R., & Wink, J. E. 1990, A&A, 228, 95Müller, H. S. P. 2010, A&A, 514, L6Müller, H. S. P., Klein, H., Belov, S. P., et al. 1999, J. Mol. Spectr., 195, 177Müller, H. S. P., Farhoomand, J., Cohen, E. A., et al. 2000a, J. Mol. Spectr., 201,
1Müller, H. S. P., Winnewisser, G., Demaison, J., Perrin, A., & Valentin, A.
2000b, J. Mol. Spectr., 200, 143Müller, H. S. P., Menten, K. M., & Mäder, H. 2004, A&A, 428, 1019Müller, H. S. P., Schlöder, F., Stutzki, J., & Winnewisser, G. 2005, J. Mol.
Spectr., 742, 215Mürtz, P., Zink, L. R., Evenson, K. M., & Brown, J. M. 1998, J. Chem. Phys.,
109, 9744Myers, P. C., Mardones, D., Tafalla, M., Williams, J. P., & Wilner, D. J. 1996,
ApJ, 465, L133Neill, J. L., Bergin, E. A., Lis, D. C., et al. 2012, J. Mol. Spectr., 280, 150Neufeld, D. A., & Wolfire, M. G. 2009, ApJ, 706, 1594Nolt, I. G., Radostitz, J. V., Dilonardo, G., et al. 1987, J. Mol. Spectr., 125,
274Nummelin, A., Bergman, P., Hjalmarson, Å., et al. 2000, ApJS, 128, 213Ott, S. 2010, in Astronomical Data Analysis Software and Systems XIX, eds. Y.
Mizumoto, K.-I. Morita, & M. Ohishi, ASP Conf. Ser., 434, 139Padovani, M., Walmsley, C. M., Tafalla, M., Galli, D., & Müller, H. S. P. 2009,
A&A, 505, 1199Pagani, L., Daniel, F., & Dubernet, M.-L. 2009, A&A, 494, 719Pickett, H. M., Poynter, R. L., Cohen, E. A., et al. 1998, J. Quant. Spec. Radiat.
Transf., 60, 883Pickett, H. M., Pearson, J. C., & Miller, C. E. 2005, J. Mol. Spectr., 233, 174Pilbratt, G. L., Riedinger, J. R., Passvogel, T., et al. 2010, A&A, 518, L1Roelfsema, P. R., Helmich, F. P., Teyssier, D., et al. 2012, A&A, 537, A17Schilke, P., Groesbeck, T. D., Blake, G. A., & Phillips, T. G. 1997, ApJS, 108,
301Schilke, P., Comito, C., Thorwirth, S., et al. 2006, A&A, 454, L41Shimajiri, Y., Takahashi, S., Takakuwa, S., Saito, M., & Kawabe, R. 2008, ApJ,
683, 255Shimajiri, Y., Kawabe, R., Takakuwa, S., et al. 2011, PASJ, 63, 105Snell, R. L., Howe, J. E., Ashby, M. L. N., et al. 2000, ApJ, 539, L93Takano, S., Klaus, T., & Winnewisser, G. 1998, J. Mol. Spectr., 192, 309Thorwirth, S., Müller, H. S. P., Lewen, F., Gendriesch, R., & Winnewisser, G.
2000, A&A, 363, L37Thorwirth, S., Müller, H. S. P., Lewen, F., et al. 2003, ApJ, 585, L163van der Wiel, M. H. D., Pagani, L., van der Tak, F. F. S., Kazmierczak, M., &
Ceccarelli, C. 2013, A&A, 553, A11Viti, S., Jimenez-Serra, I., Yates, J. A., et al. 2011, ApJ, 740, L3Wakelam, V., Caselli, P., Ceccarelli, C., Herbst, E., & Castets, A. 2004, A&A,
422, 159Wakelam, V., Ceccarelli, C., Castets, A., et al. 2005, A&A, 437, 149Wampfler, S. F., Herczeg, G. J., Bruderer, S., et al. 2010, A&A, 521, L36Winnewisser, G., Belov, S. P., Klaus, T., & Schieder, R. 1997, J. Mol. Spectr.,
184, 468Yu, S., Pearson, J. C., Drouin, B. J., et al. 2010, J. Chem. Phys., 133, 174317Zernickel, A., Schilke, P., Schmiedeke, A., et al. 2012, A&A, 546, A87
Pages 19 to 36 are available in the electronic edition of the journal at http://www.aanda.org
A57, page 18 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Appendix A: Detected transitions
In Table A.1, we present a frequency-sorted table of the tran-sitions detected in the survey. In the first six columns, we givethe database properties of each transition. Columns 7−10 givethe Gaussian fit velocity and width, and their associated formaluncertainties. Columns 11−14 give the peak and integrated in-tensity, and associated uncertainty. Blending is indicated in col-umn 15, by a B: followed by an identification of the blended line(only one B: line is given also for multiple overlapping blends).Line profile parameters (vlsr, FWHM, Tmb) are not given for thelines which are blended. For some species, such as OH and SH+,the line parameters were determined by fitting models of the hy-perfine line profile to the data, these results can be seen in Table 2and Fig. 3 and plotted with red dashed lines in figures showingexamples of the data.
A57, page 19 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.Tra
nsiti
ons
dete
cted
inth
eH
IFIs
pect
rals
urve
yof
OM
C-2
FIR
4.
Gau
ssia
nfit
From
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
480.
269
CH
3OH
3 2−
3 148
0.26
951
.64
4.89
e-04
12.2
60.
185.
200.
420.
1722
1.01
0.04
481.
504
CH
3OH
2 2−
2 148
1.50
444
.67
3.94
e-04
11.3
60.
143.
640.
340.
1423
0.42
0.04
481.
916
C34
S10
0−9 0
481.
916
127.
232.
38e-
0310
.01
0.10
1.68
0.24
0.05
190.
210.
0348
2.28
2C
H3O
H10
0−9 0
482.
282
140.
605.
02e-
0411
.80
0.06
3.61
0.13
0.37
161.
930.
0348
2.95
9C
H3O
H10−
1−9 −
148
2.95
913
3.15
5.00
e-04
11.8
20.
023.
820.
040.
6415
3.09
0.03
483.
141
CH
3OH
100−
9 048
3.14
112
7.60
5.05
e-04
11.7
30.
023.
720.
040.
6817
3.48
0.04
483.
389
CH
3OH
102−
9 248
3.38
916
5.35
4.89
e-04
12.2
20.
125.
070.
270.
1220
0.81
0.04
483.
472
CH
3OH
10−
4−9 −
448
3.47
221
5.55
6.30
e-04
12.6
50.
255.
210.
700.
0415
0.18
0.02
483.
539
CH
3OH
104−
9 448
3.53
920
7.99
6.31
e-04
14B
:CH
3OH
(10 4−
9 4)
483.
539
CH
3OH
104−
9 448
3.53
920
7.99
6.31
e-04
14B
:CH
3OH
(10 4−
9 4)
483.
551
CH
3OH
103−
9 348
3.55
117
7.46
6.82
e-04
14B
:CH
3OH
(10 4−
9 4)
483.
556
CH
3OH
10−
3−9 −
348
3.55
619
0.37
6.87
e-04
14B
:CH
3OH
(10 4−
9 4)
483.
566
CH
3OH
103−
9 348
3.56
617
7.46
6.82
e-04
14B
:CH
3OH
(10 4−
9 4)
483.
686
CH
3OH
101−
9 148
3.68
614
8.73
7.60
e-04
13B
:CH
3OH
(10 3−
9 3)
483.
697
CH
3OH
103−
9 348
3.69
717
5.39
6.85
e-04
13B
:CH
3OH
(10 1−
9 1)
483.
761
CH
3OH
102−
9 248
3.76
116
5.40
4.90
e-04
12.1
60.
114.
090.
260.
1116
0.51
0.02
484.
005
CH
3OH
2 2−
2 148
4.00
544
.67
4.01
e-04
14B
:CH
3OH
(10 2−
9 2)
484.
023
CH
3OH
102−
9 248
4.02
314
9.97
4.83
e-04
12B
:CH
3OH
(22−
2 1)
484.
072
CH
3OH
10−
2−9 −
248
4.07
215
3.63
4.89
e-04
11.9
20.
064.
250.
140.
1813
0.94
0.02
485.
263
CH
3OH
3 2−
3 148
5.26
351
.64
5.05
e-04
11.7
40.
034.
330.
060.
2016
1.10
0.03
485.
418
H2C
l+1 1
,1,5/2−
0 0,0,3/2
485.
418
23.3
01.
59e-
038.
260.
162.
820.
38−
0.03
11−
0.18
0.01
486.
941
CH
3OH
4 2−
4 148
6.94
160
.92
5.51
e-04
11.5
70.
034.
400.
060.
2416
1.27
0.03
487.
532
CH
3OH
101−
9 148
7.53
214
3.28
5.15
e-04
12.0
20.
023.
840.
050.
3817
2.00
0.03
489.
037
CH
3OH
5 2−
5 148
9.03
772
.53
5.79
e-04
11.9
00.
033.
880.
080.
2317
1.27
0.04
489.
751
CS
10−
948
9.75
112
9.29
2.51
e-03
11.8
50.
098.
280.
210.
5117
4.34
0.04
491.
551
CH
3OH
6 2−
6 149
1.55
186
.46
6.00
e-04
11.8
80.
064.
650.
150.
2118
1.11
0.04
491.
935
SO2
7 4,4−
6 3,3
491.
935
65.0
19.
49e-
0417
B:H
2CO
(71,
7−6 1
,6)
491.
968
H2C
O7 1
,7−
6 1,6
491.
968
106.
313.
44e-
0318
B:S
O2
(74,
4−6 3
,3)
492.
161
C1−
049
2.16
123
.62
7.99
e-08
11.9
00.
021.
810.
051.
3018
4.74
0.04
492.
279
CH
3OH
4 1−
3 049
2.27
937
.55
3.83
e-04
11.6
90.
024.
150.
040.
6617
3.47
0.04
493.
699
CH
3OH
5 3−
4 249
3.69
984
.62
6.62
e-04
11.6
70.
023.
720.
050.
4914
2.44
0.03
493.
734
CH
3OH
5 3−
4 249
3.73
484
.62
6.62
e-04
11.5
90.
023.
710.
050.
5015
2.56
0.03
494.
455
NH
2D1 1
,0,1−
0 0,0,0
494.
455
23.7
39.
95e-
0411
.19
0.03
2.21
0.08
0.14
140.
420.
0249
4.48
2C
H3O
H7 2−
7 149
4.48
210
2.70
6.18
e-04
11.7
90.
025.
060.
060.
2114
1.30
0.03
495.
173
CH
3OH
7 0−
6 −1
495.
173
78.0
83.
21e-
0411
.71
0.02
3.68
0.05
0.40
151.
940.
0349
6.92
4C
H3O
H14
0−13
149
6.92
425
6.14
3.26
e-04
12.3
40.
144.
620.
320.
0813
0.35
0.03
497.
828
CH
3OH
8 2−
8 149
7.82
812
1.27
6.36
e-04
11.9
00.
044.
610.
080.
2014
1.29
0.03
501.
589
CH
3OH
9 2−
9 150
1.58
914
2.15
6.54
e-04
11.9
30.
073.
980.
150.
1614
0.87
0.03
504.
294
CH
3OH
7 1−
6 050
4.29
486
.05
3.53
e-04
11.7
20.
024.
010.
060.
3915
2.09
0.03
Not
es.T
hefir
stsi
xco
lum
nsgi
veth
eda
taba
sepr
oper
ties
ofea
chtr
ansi
tion.
Col
umns
7−10
give
the
Gau
ssia
nfit
velo
city
and
wid
th,a
ndth
eira
ssoc
iate
dfo
rmal
unce
rtai
ntie
s.C
olum
ns11−
14gi
veth
epe
akan
din
tegr
ated
inte
nsity
,and
asso
ciat
edun
cert
aint
y.B
lend
ing
isin
dica
ted
inC
ol.1
5,by
aB:
follo
wed
byan
iden
tifica
tion
ofth
ebl
ende
dlin
e(o
nly
oneB:
line
isgi
ven
also
for
mul
tiple
over
lapp
ing
blen
ds).
Lin
epr
ofile
para
met
ers
(vls
r,FW
HM
,Tm
b)ar
eno
tgiv
enfo
rthe
lines
whi
char
ebl
ende
d.Fo
rsom
esp
ecie
s,su
chas
OH
and
SH+,t
helin
epa
ram
eter
sw
ere
dete
rmin
edby
fittin
gm
odel
sof
the
hype
rfine
line
profi
leto
the
data
,the
sere
sults
are
plot
ted
with
red
dash
edlin
esin
figur
essh
owin
gex
ampl
esof
the
data
.
A57, page 20 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
505.
565
H2S
2 2,1−
2 1,2
505.
565
79.3
72.
40e-
0411
.29
0.04
3.83
0.10
0.11
160.
480.
0350
5.76
2C
H3O
H10
2−10
150
5.76
216
5.35
6.73
e-04
11.9
50.
034.
160.
070.
1418
0.62
0.03
505.
834
H2C
O7 0
,7−
6 0,6
505.
834
97.4
43.
82e-
0311
.75
0.02
4.42
0.04
0.74
184.
030.
0450
6.15
3C
H3O
H11
1−10
250
6.15
317
4.27
2.34
e-04
12.0
50.
144.
160.
320.
0918
0.32
0.03
506.
825
DC
N7−
650
6.82
597
.30
6.33
e-03
12.0
40.
376.
780.
870.
0415
0.24
0.03
509.
146
H2C
O7 2
,6−
6 2,5
509.
146
144.
933.
58e-
0311
.70
0.02
4.51
0.05
0.39
162.
280.
0350
9.29
2H
DO
1 1,0−
1 0,1
509.
292
46.7
62.
32e-
0316
B:H
2CO
(76,
1−6 6
,0)
509.
306
H2C
O7 6
,1−
6 6,0
509.
306
520.
811.
03e-
0317
B:H
DO
(11,
0−1 0
,1)
509.
306
H2C
O7 6
,2−
6 6,1
509.
306
520.
811.
03e-
0316
B:H
DO
(11,
0−1 0
,1)
509.
562
H2C
O7 5
,3−
6 5,2
509.
562
391.
841.
91e-
0317
B:H
2CO
(75,
2−6 5
,1)
509.
562
H2C
O7 5
,2−
6 5,1
509.
562
391.
841.
91e-
0317
B:H
2CO
(75,
3−6 5
,2)
509.
565
CH
3OH
102−
9 150
9.56
514
9.97
4.07
e-04
17B
:H2C
O(7
5,3−
6 5,2
)50
9.83
0H
2CO
7 4,4−
6 4,3
509.
830
286.
172.
63e-
0319
B:H
2CO
(74,
3−6 4
,2)
509.
830
H2C
O7 4
,3−
6 4,2
509.
830
286.
172.
63e-
0319
B:H
2CO
(74,
4−6 4
,3)
510.
156
H2C
O7 3
,5−
6 3,4
510.
156
203.
893.
20e-
0311
.88
0.02
4.08
0.04
0.55
162.
890.
0351
0.23
8H
2CO
7 3,4−
6 3,3
510.
238
203.
903.
20e-
0311
.93
0.02
4.19
0.04
0.54
162.
770.
0351
0.34
5C
H3O
H11
2−11
151
0.34
519
0.86
6.94
e-04
12.0
20.
104.
280.
240.
1015
0.44
0.03
512.
427
NH
2D2 0
,2,1−
1 1,0,0
512.
427
47.7
51.
57e-
0411
.49
0.09
3.00
0.22
0.07
170.
190.
0351
3.07
6H
2CO
7 2,5−
6 2,4
513.
076
145.
353.
66e-
0311
.92
0.02
4.40
0.05
0.39
182.
260.
0351
4.85
3SO
1211−
1110
514.
853
167.
591.
82e-
039.
300.
0812
.17
0.19
0.06
160.
680.
0451
5.17
0C
H3O
H16
0−15
151
5.17
031
5.21
4.10
e-04
12.0
50.
084.
310.
180.
2217
1.08
0.04
515.
335
CH
3OH
122−
121
515.
335
218.
697.
16e-
0412
.57
0.15
5.69
0.34
0.09
150.
530.
0351
6.33
5SO
1212−
1111
516.
335
174.
221.
83e-
039.
320.
067.
380.
150.
0616
0.45
0.03
517.
354
SO12
13−
1112
517.
354
165.
781.
86e-
039.
050.
0612
.09
0.14
0.07
170.
730.
0451
7.97
0H
13C
N6−
551
7.97
087
.01
6.65
e-03
12.1
40.
058.
870.
110.
1116
0.96
0.03
519.
188
SO2
291,
29−
280,
2851
9.18
837
9.20
1.91
e-03
11.5
00.
4212
.03
1.00
0.02
160.
270.
0352
0.17
9C
H3O
H2 −
2−1 −
152
0.17
932
.86
9.76
e-04
11.7
80.
054.
780.
110.
4317
2.39
0.03
520.
460
H13
CO
+6−
552
0.46
087
.43
1.14
e-02
11.3
80.
042.
420.
090.
1216
0.45
0.03
520.
728
CH
3OH
132−
131
520.
728
248.
847.
40e-
0411
.73
0.13
2.85
0.31
0.08
190.
490.
0352
2.07
7N
D1 2
,3,4−
0 1,2,3
522.
077
25.0
61.
07e-
0311
.17
0.11
10.6
70.
260.
0316
0.27
0.02
523.
274
CH
3OH
14−
1−13
052
3.27
424
8.93
6.27
e-04
11.9
10.
023.
700.
040.
3517
1.63
0.04
523.
972
CC
H6 1
3/2,
7−5 1
1/2,
652
3.97
288
.02
4.58
e-04
18B
:CC
H(6
13/2,6−
5 11/
2,5)
523.
972
CC
H6 1
3/2,
6−5 1
1/2,
552
3.97
288
.02
4.53
e-04
17B
:CC
H(6
13/2,7−
5 11/
2,6)
524.
003
CH
3OH
15−
4−15−
352
4.00
336
6.32
1.06
e-03
13.4
60.
132.
910.
300.
0316
0.13
0.02
524.
034
CC
H6 1
1/2,
6−5 9
/2,5
524.
034
88.0
44.
51e-
0418
B:C
CH
(611/2,5−
5 9/2,4
)52
4.03
5C
CH
6 11/
2,5−
5 9/2,4
524.
035
88.0
44.
43e-
0418
B:C
CH
(611/2,6−
5 9/2,5
)52
4.26
9C
H3O
H13−
4−13−
352
4.26
929
9.06
7.10
e-04
11.2
70.
213.
180.
500.
0416
0.27
0.03
524.
385
CH
3OH
12−
4−12−
352
4.38
526
8.91
7.03
e-04
11.7
50.
569.
291.
320.
0417
0.30
0.03
524.
489
CH
3OH
11−
4−11−
352
4.48
924
1.07
6.94
e-04
12.5
80.
235.
520.
530.
0517
0.29
0.03
524.
666
CH
3OH
9 −4−
9 −3
524.
666
192.
346.
64e-
0411
.60
0.12
3.35
0.29
0.06
160.
250.
0252
4.74
0C
H3O
H8 −
4−8 −
352
4.74
017
1.46
6.39
e-04
12.1
10.
065.
900.
130.
0816
0.46
0.03
524.
805
CH
3OH
7 −4−
7 −3
524.
805
152.
906.
03e-
0411
.85
0.04
4.81
0.10
0.08
170.
490.
0252
4.86
1C
H3O
H6 −
4−6 −
352
4.86
113
6.65
5.49
e-04
11.7
90.
133.
960.
320.
1015
0.56
0.02
524.
908
CH
3OH
5 −4−
5 −3
524.
908
122.
724.
62e-
0412
.01
0.16
3.85
0.38
0.08
150.
400.
02
A57, page 21 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
524.
947
CH
3OH
4 −4−
4 −3
524.
947
111.
123.
08e-
0411
.81
0.14
4.16
0.33
0.06
160.
240.
0252
5.66
6H
2CO
7 1,6−
6 1,5
525.
666
112.
794.
20e-
0311
.82
0.01
4.92
0.03
1.22
167.
140.
0352
6.03
9SH
+1 2
,3/2−
0 1,1/2
526.
039
25.2
57.
99e-
0413
B:S
H+
(12,
5/2−
0 1,3/2
)52
6.04
8SH
+1 2
,5/2−
0 1,3/2
526.
048
25.2
59.
59e-
0413
B:S
H+
(12,
3/2−
0 1,1/2
)52
6.52
0C
H3O
H14
2−14
152
6.52
028
1.29
7.66
e-04
12.5
10.
075.
670.
160.
0613
0.37
0.02
527.
053
CH
3OH
111−
101
527.
053
166.
376.
54e-
0411
.97
0.04
3.86
0.10
0.31
161.
410.
0352
7.17
1C
H3O
H15
3−15
252
7.17
132
6.28
8.92
e-04
13.0
70.
384.
810.
890.
0317
0.14
0.02
527.
658
CH
3OH
143−
142
527.
658
291.
468.
88e-
0411
.99
0.36
8.39
0.86
0.04
170.
340.
0352
8.17
7C
H3O
H13
3−13
252
8.17
725
8.96
8.81
e-04
12.5
10.
153.
740.
360.
0517
0.24
0.03
528.
683
CH
3OH
123−
122
528.
683
228.
788.
74e-
0412
.10
0.21
4.01
0.50
0.05
170.
250.
0352
9.14
3C
H3O
H11
3−11
252
9.14
320
0.92
8.64
e-04
12.5
30.
144.
110.
330.
0715
0.37
0.03
529.
540
CH
3OH
103−
102
529.
540
175.
398.
52e-
0412
.15
0.12
5.06
0.29
0.09
160.
480.
0352
9.86
7C
H3O
H9 3−
9 252
9.86
715
2.17
8.37
e-04
12.3
70.
045.
200.
100.
1116
0.64
0.03
530.
123
CH
3OH
8 3−
8 253
0.12
313
1.28
8.18
e-04
11.8
10.
094.
890.
200.
1114
0.63
0.02
530.
184
CH
3OH
110−
100
530.
184
166.
056.
69e-
0412
.00
0.04
3.72
0.11
0.38
161.
800.
0353
0.31
6C
H3O
H7 3−
7 253
0.31
611
2.71
7.93
e-04
12.3
30.
084.
760.
200.
1615
0.74
0.03
530.
455
CH
3OH
6 3−
6 253
0.45
596
.46
7.58
e-04
12.1
30.
074.
780.
160.
1613
0.78
0.02
530.
549
CH
3OH
5 3−
5 253
0.54
982
.53
7.04
e-04
12.1
70.
095.
770.
220.
1613
0.91
0.02
530.
610
CH
3OH
4 3−
4 253
0.61
070
.93
6.14
e-04
12.1
80.
035.
040.
070.
1414
0.79
0.02
530.
647
CH
3OH
3 3−
3 253
0.64
761
.64
4.37
e-04
12.3
70.
126.
050.
280.
1215
0.78
0.03
531.
079
CH
3OH
11−
1−10−
153
1.07
915
8.64
6.69
e-04
11.8
90.
043.
980.
090.
6914
3.48
0.03
531.
319
CH
3OH
110−
100
531.
319
153.
106.
75e-
0411
.87
0.02
4.02
0.04
0.74
183.
670.
0353
1.63
6C
H3O
H11
2−10
253
1.63
619
0.87
6.58
e-04
12.2
50.
024.
230.
060.
1419
0.70
0.03
531.
716
HC
N6−
553
1.71
689
.32
7.20
e-03
12.0
40.
059.
010.
122.
2319
21.0
70.
0553
1.77
2C
H3O
H11−
4−10−
453
1.77
224
1.07
8.70
e-04
12.5
60.
315.
970.
750.
0417
0.15
0.01
531.
829
CH
3OH
114−
104
531.
829
249.
188.
75e-
0412
.27
0.56
5.90
1.33
0.03
180.
130.
0253
1.86
6C
H3O
H11−
3−10−
353
1.86
621
5.90
9.34
e-04
17B
:CH
3OH
(11 3−
103)
531.
869
CH
3OH
113−
103
531.
869
202.
989.
27e-
0417
B:C
H3O
H(1
1 −3−
10−
3)53
1.87
0C
H3O
H11
4−10
453
1.87
023
3.52
8.72
e-04
16B
:CH
3OH
(11 −
3−10−
3)53
1.87
1C
H3O
H11
4−10
453
1.87
123
3.52
8.72
e-04
15B
:CH
3OH
(11 −
3−10−
3)53
1.89
3C
H3O
H11
3−10
353
1.89
320
2.98
6.26
e-04
18B
:CH
3OH
(11 −
3−10−
3)53
2.03
1C
H3O
H11
1−10
153
2.03
117
4.27
6.86
e-04
11.9
40.
034.
000.
070.
2717
1.37
0.03
532.
069
CH
3OH
113−
103
532.
069
200.
926.
28e-
0411
.98
0.08
4.38
0.20
0.09
160.
480.
0253
2.13
3C
H3O
H11
2−10
253
2.13
319
0.94
6.60
e-04
11.7
70.
043.
680.
100.
1215
0.45
0.02
532.
466
CH
3OH
112−
102
532.
466
175.
536.
51e-
0412
.00
0.02
4.14
0.04
0.37
141.
750.
0353
2.56
7C
H3O
H11−
2−10−
253
2.56
717
9.19
6.58
e-04
12.0
00.
033.
740.
060.
1914
0.92
0.02
532.
707
CH
3OH
152−
151
532.
707
316.
051.
18e-
0317
B:C
H(2 Π
1 1,0,3/2,1−
1 −1,
0,1/
2,1)
532.
722
CH
2 Π1 1
,0,3/2,1−
1 −1,
0,1/
2,1
532.
722
25.7
32.
07e-
0419
B:C
H(2 Π
1 1,0,3/2,2−
1 −1,
0,1/
2,1)
532.
724
CH
2 Π1 1
,0,3/2,2−
1 −1,
0,1/
2,1
532.
724
25.7
36.
21e-
0419
B:C
H(2 Π
1 1,0,3/2,1−
1 −1,
0,1/
2,1)
535.
062
HC
O+
6−5
535.
062
89.8
81.
25e-
0211
.46
0.03
3.81
0.07
4.27
1422
.76
0.04
536.
191
CH
3OH
111−
101
536.
191
169.
016.
89e-
0412
.01
0.02
4.05
0.04
0.44
152.
230.
0353
6.76
1C
H2 Π
1 −1,
0,3/
2,2−
1 1,0,1/2,1
536.
761
25.7
66.
38e-
0412
.74
0.08
2.48
0.18
0.06
180.
210.
0253
8.57
1C
H3O
H5 1−
4 053
8.57
149
.06
4.93
e-04
11.8
00.
024.
470.
040.
7814
4.19
0.03
538.
689
CS
11−
1053
8.68
915
5.15
3.35
e-03
12.2
10.
079.
380.
170.
4514
4.07
0.03
A57, page 22 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Tabl
eA
.1.c
ontin
ued.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
539.
282
CH
3OH
162−
161
539.
282
353.
128.
24e-
0412
.33
0.28
4.79
0.73
0.03
120.
220.
0254
0.92
2C
H3O
H15
0−14
154
0.92
229
0.74
4.21
e-04
12.6
30.
054.
120.
120.
0717
0.35
0.03
542.
001
CH
3OH
6 3−
5 254
2.00
198
.55
7.93
e-04
11.8
50.
023.
990.
050.
5415
2.73
0.03
542.
082
CH
3OH
6 3−
5 254
2.08
298
.55
7.93
e-04
11.7
90.
023.
990.
040.
5414
2.60
0.02
543.
076
CH
3OH
8 0−
7 −1
543.
076
96.6
14.
54e-
0411
.89
0.02
3.92
0.05
0.45
132.
310.
0354
3.89
8H
NC
6 0,0−
5 0,0
543.
898
91.3
78.
04e-
0311
.54
0.04
2.20
0.09
0.38
141.
620.
0254
6.23
9C
H3O
H17
2−17
154
6.23
939
2.50
1.27
e-03
12.0
60.
868.
992.
100.
0316
0.17
0.02
547.
676
H218
O1 1
,0−
1 0,1
547.
676
60.4
63.
29e-
0313
.69
0.08
19.1
90.
200.
0719
1.09
0.05
548.
831
C18
O5−
454
8.83
179
.02
1.06
e-05
11.3
40.
012.
020.
031.
3616
5.10
0.03
550.
926
13C
O5−
455
0.92
679
.33
1.07
e-05
11.6
00.
023.
090.
046.
9416
31.3
30.
0455
3.14
6C
H3O
H8 1−
7 055
3.14
610
4.62
4.63
e-04
11.7
30.
024.
200.
060.
3816
1.82
0.03
554.
055
CH
3OH
121−
112
554.
055
202.
124.
63e-
0412
.09
0.10
3.28
0.23
0.08
150.
410.
0255
6.93
6H
2O1 1
,0,0−
1 0,1,0
556.
936
60.9
63.
46e-
0311
.36
0.04
20.5
40.
102.
1219
33.7
20.
0655
8.08
7SO
1312−
1211
558.
087
194.
372.
32e-
039.
780.
079.
170.
170.
0720
0.59
0.04
558.
345
CH
3OH
112−
101
558.
345
175.
535.
16e-
0412
.10
0.02
3.66
0.05
0.39
171.
760.
0355
8.96
7N
2H+
6−5
558.
967
93.9
01.
16e-
0211
.55
0.01
2.24
0.02
2.28
167.
710.
0355
9.31
9SO
1313−
1212
559.
319
201.
072.
34e-
039.
980.
085.
490.
190.
0516
0.40
0.03
560.
178
SO13
14−
1213
560.
178
192.
662.
37e-
0310
.93
0.07
11.1
50.
170.
0517
0.60
0.04
561.
712
C17
O5 5
/2−
4 7/2
561.
712
80.8
81.
20e-
0711
.18
0.02
2.52
0.05
0.35
151.
580.
0356
1.89
9H
2CO
8 1,8−
7 1,7
561.
899
133.
285.
20e-
0311
.98
0.02
4.74
0.04
1.47
378.
380.
0856
6.73
0C
N5 9
/2,1
1/2−
4 7/2,9/2
566.
730
81.5
91.
98e-
0316
B:C
N(5
9/2,
7/2−
4 7/2,5/2
)56
6.73
1C
N5 9
/2,7/2−
4 7/2,5/2
566.
731
81.5
91.
86e-
0316
B:C
N(5
9/2,
11/2−
4 7/2,9/2
)56
6.73
1C
N5 9
/2,9/2−
4 7/2,7/2
566.
731
81.5
91.
88e-
0316
B:C
N(5
9/2,
11/2−
4 7/2,9/2
)56
6.94
7C
N5 1
1/2,
11/2−
4 9/2,9/2
566.
947
81.6
41.
96e-
0318
B:C
N(5
11/2,1
3/2−
4 9/2,1
1/2)
566.
947
CN
5 11/
2,13/2−
4 9/2,1
1/2
566.
947
81.6
42.
03e-
0324
B:C
N(5
11/2,1
1/2−
4 9/2,9/2
)56
6.94
7C
N5 1
1/2,
9/2−
4 9/2,7/2
566.
947
81.6
51.
95e-
0316
B:C
N(5
11/2,1
1/2−
4 9/2,9/2
)56
8.56
6C
H3O
H3 −
2−2 −
156
8.56
639
.83
1.01
e-03
11.9
00.
054.
960.
120.
5116
2.87
0.03
568.
783
CH
3OH
170−
161
568.
783
354.
545.
62e-
0412
.09
0.03
3.84
0.07
0.20
151.
000.
0357
2.11
315
NH
31 0
,0−
0 0,1
572.
113
28.0
01.
57e-
0312
.83
0.38
5.76
0.90
0.02
130.
150.
0257
2.49
8o-
NH
31 0
,0−
0 0,1
572.
498
27.4
81.
57e-
0311
.79
0.02
5.28
0.04
1.76
1410
.80
0.03
572.
899
CH
3OH
15−
1−14
057
2.89
928
3.64
8.61
e-04
12.0
20.
023.
920.
040.
3114
1.55
0.03
574.
868
CH
3OH
121−
111
574.
868
193.
968.
53e-
0412
.24
0.02
4.44
0.04
0.28
131.
480.
0257
6.26
8C
O5−
457
6.26
882
.98
1.22
e-05
11.3
70.
1411
.91
0.32
15.3
620
171.
010.
0757
6.70
8H
2CO
8 0,8−
7 0,7
576.
708
125.
125.
70e-
0311
.94
0.02
4.76
0.04
0.59
133.
320.
0357
8.00
6C
H3O
H12
0−11
057
8.00
619
3.79
8.70
e-04
12.1
20.
023.
900.
040.
4013
1.87
0.02
579.
085
CH
3OH
2 2−
1 157
9.08
544
.67
1.23
e-03
11.8
00.
024.
710.
050.
3914
2.15
0.02
579.
151
CH
3OH
12−
1−11−
157
9.15
118
6.43
8.72
e-04
12.0
60.
023.
770.
050.
7213
3.43
0.02
579.
201
DC
N8−
757
9.20
112
5.10
9.52
e-03
12.0
40.
202.
930.
480.
0312
0.11
0.01
579.
460
CH
3OH
120−
110
579.
460
180.
918.
79e-
0411
.96
0.02
3.98
0.04
0.72
123.
470.
0257
9.85
8C
H3O
H12
2−11
257
9.85
821
8.69
8.62
e-04
12.2
60.
084.
670.
180.
1413
0.80
0.02
579.
921
CH
3OH
2 2−
1 157
9.92
144
.67
1.24
e-03
11.7
10.
075.
070.
150.
3913
2.31
0.02
580.
033
CH
3OH
12−
5−11−
558
0.03
330
5.00
1.08
e-03
14B
:CH
3OH
(12 5−
115)
580.
058
CH
3OH
125−
115
580.
058
318.
901.
09e-
0313
B:C
H3O
H(1
2 −5−
11−
5)58
0.05
8C
H3O
H12
5−11
558
0.05
831
8.90
1.09
e-03
13B
:CH
3OH
(12 −
5−11−
5)58
0.05
9C
H3O
H12−
4−11−
458
0.05
926
8.91
1.16
e-03
14B
:CH
3OH
(12 −
5−11−
5)
A57, page 23 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
580.
126
CH
3OH
124−
114
580.
126
277.
021.
17e-
0316
B:C
H3O
H(1
2 −3−
11−
3)58
0.16
3C
H3O
H12−
3−11−
358
0.16
324
3.74
1.23
e-03
14B
:CH
3OH
(12 4−
114)
580.
176
CH
3OH
123−
113
580.
176
230.
831.
22e-
0313
B:C
H3O
H(1
2 −3−
11−
3)58
0.19
5C
H3O
H12
4−11
458
0.19
526
1.37
1.16
e-03
17B
:CH
3OH
(12 −
3−11−
3)58
0.19
6C
H3O
H12
4−11
458
0.19
626
1.37
1.16
e-03
16B
:CH
3OH
(12 −
3−11−
3)58
0.21
3C
H3O
H12
3−11
358
0.21
323
0.83
1.22
e-03
15B
:CH
3OH
(12 4−
114)
580.
369
CH
3OH
121−
111
580.
369
202.
128.
94e-
0412
.02
0.02
4.16
0.04
0.25
151.
330.
0358
0.44
2C
H3O
H12
3−11
358
0.44
222
8.78
8.29
e-04
11.9
90.
054.
510.
120.
0716
0.37
0.02
580.
502
CH
3OH
122−
112
580.
502
218.
808.
64e-
0412
.10
0.03
3.95
0.08
0.13
150.
540.
0258
0.90
3C
H3O
H12
2−11
258
0.90
320
3.41
8.53
e-04
11.9
40.
024.
060.
040.
3614
1.84
0.03
581.
092
CH
3OH
12−
2−11−
258
1.09
220
7.08
8.63
e-04
12.0
20.
034.
770.
060.
1915
1.10
0.03
581.
612
H2C
O8 2
,7−
7 2,6
581.
612
172.
845.
49e-
0311
.83
0.02
4.42
0.04
0.34
161.
740.
0358
1.75
0H
2CO
8 7,2−
7 7,1
581.
750
700.
861.
37e-
0317
B:H
2CO
(87,
1−7 7
,0)
581.
750
H2C
O8 7
,1−
7 7,0
581.
750
700.
861.
37e-
0317
B:H
2CO
(87,
2−7 7
,1)
582.
071
H2C
O8 6
,3−
7 6,2
582.
071
548.
742.
57e-
0314
B:H
2CO
(86,
2−7 6
,1)
582.
071
H2C
O8 6
,2−
7 6,1
582.
071
548.
742.
57e-
0315
B:H
2CO
(86,
3−7 6
,2)
582.
382
H2C
O8 5
,4−
7 5,3
582.
382
419.
793.
58e-
0315
B:H
2CO
(85,
3−7 5
,2)
582.
382
H2C
O8 5
,3−
7 5,2
582.
382
419.
793.
58e-
0316
B:H
2CO
(85,
4−7 5
,3)
582.
723
H2C
O8 4
,5−
7 4,4
582.
723
314.
144.
42e-
0318
B:H
2CO
(84,
4−7 4
,3)
582.
724
H2C
O8 4
,4−
7 4,3
582.
724
314.
144.
42e-
0318
B:H
2CO
(84,
5−7 4
,4)
583.
145
H2C
O8 3
,6−
7 3,5
583.
145
231.
885.
07e-
0312
.02
0.02
4.38
0.04
0.48
162.
600.
0358
3.30
9H
2CO
8 3,5−
7 3,4
583.
309
231.
895.
08e-
0311
.96
0.02
4.60
0.04
0.48
172.
700.
0358
4.14
7C
H3O
H16
0−15
158
4.14
732
7.63
7.81
e-04
12.5
10.
134.
520.
320.
0717
0.32
0.03
584.
450
CH
3OH
6 1−
5 058
4.45
062
.87
6.25
e-04
11.9
80.
024.
280.
040.
9316
4.59
0.03
584.
822
CH
3OH
121−
111
584.
822
197.
088.
98e-
0412
.03
0.02
4.09
0.04
0.44
182.
220.
0358
7.45
4H
2CO
8 2,6−
7 2,5
587.
454
173.
555.
66e-
0311
.96
0.02
4.35
0.05
0.31
161.
680.
0358
7.61
6C
S12−
1158
7.61
618
3.35
4.36
e-03
12.1
90.
0810
.32
0.20
0.36
173.
750.
0459
0.27
8C
H3O
H7 3−
6 259
0.27
811
4.79
9.50
e-04
11.7
80.
024.
080.
040.
5516
2.52
0.03
590.
440
CH
3OH
7 3−
6 259
0.44
011
4.79
9.50
e-04
11.8
40.
024.
130.
040.
5415
2.67
0.03
590.
791
CH
3OH
9 0−
8 −1
590.
791
117.
466.
23e-
0412
.01
0.02
4.15
0.04
0.49
162.
540.
0359
9.92
7H
DO
2 1,1−
2 0,2
599.
927
95.2
33.
45e-
0312
.03
0.09
5.05
0.21
0.04
150.
250.
0260
0.33
1H
2CO
8 1,7−
7 1,6
600.
331
141.
616.
34e-
0312
.00
0.01
5.14
0.03
1.05
176.
120.
0360
1.25
8SO
1413−
1312
601.
258
223.
232.
92e-
037.
390.
5211
.75
1.22
0.04
170.
360.
0360
1.84
9C
H3O
H13
1−12
260
1.84
923
2.29
4.07
e-04
11.9
10.
175.
350.
400.
0915
0.58
0.03
602.
233
CH
3OH
9 1−
8 060
2.23
312
5.52
5.95
e-04
11.8
60.
023.
840.
050.
3719
1.68
0.03
602.
292
SO14
14−
1313
602.
292
229.
972.
93e-
039.
580.
088.
560.
190.
0417
0.27
0.02
603.
021
SO14
15−
1314
603.
021
221.
612.
96e-
038.
390.
109.
410.
240.
0314
0.32
0.02
604.
268
H13
CN
7−6
604.
268
116.
011.
07e-
0213
.24
0.10
11.1
00.
240.
0716
0.62
0.04
607.
175
H13
CO
+7−
660
7.17
511
6.57
1.84
e-02
11.4
80.
032.
070.
080.
0817
0.24
0.02
607.
216
CH
3OH
122−
111
607.
216
203.
416.
42e-
0412
.07
0.02
3.75
0.05
0.32
161.
430.
0361
1.26
7C
CH
7 15/
2,7−
6 13/
2,6
611.
267
117.
357.
29e-
0415
B:C
CH
(715/2,8−
6 13/
2,7)
611.
267
CC
H7 1
5/2,
8−6 1
3/2,
761
1.26
711
7.36
7.36
e-04
15B
:CC
H(7
15/2,7−
6 13/
2,6)
611.
330
CC
H7 1
3/2,
7−6 1
1/2,
661
1.33
011
7.38
7.27
e-04
16B
:CC
H(7
13/2,6−
6 11/
2,5)
611.
330
CC
H7 1
3/2,
6−6 1
1/2,
561
1.33
011
7.38
7.18
e-04
15B
:CC
H(7
13/2,7−
6 11/
2,6)
A57, page 24 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Tabl
eA
.1.c
ontin
ued.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
616.
980
CH
3OH
4 −2−
3 −1
616.
980
49.1
21.
11e-
0312
.00
0.05
5.09
0.13
0.54
123.
160.
0262
0.30
4H
CN
7−6
620.
304
119.
091.
16e-
0212
.26
0.01
10.1
30.
032.
0312
21.2
30.
0362
2.56
8C
H3O
H18
0−17
162
2.56
839
6.17
7.52
e-04
12.2
20.
034.
980.
060.
1814
1.07
0.02
622.
659
CH
3OH
131−
121
622.
659
223.
851.
09e-
0312
.33
0.02
4.62
0.05
0.29
141.
570.
0262
2.77
4C
H3O
H16−
1−15
062
2.77
432
0.63
1.16
e-03
12.1
60.
024.
180.
050.
2915
1.50
0.03
624.
208
HC
O+
7−6
624.
208
119.
842.
01e-
0211
.36
0.01
4.32
0.03
3.72
1621
.10
0.05
624.
964
H37
Cl
1 3/2−
0 3/2
624.
964
29.9
91.
16e-
0315
B:H
37C
l(1 5
/2−
0 3/2
)62
4.97
8H
37C
l1 5
/2−
0 3/2
624.
978
29.9
91.
16e-
0314
B:H
37C
l(1 3
/2−
0 3/2
)62
4.98
8H
37C
l1 1
/2−
0 3/2
624.
988
30.0
01.
16e-
0315
B:H
37C
l(1 5
/2−
0 3/2
)62
5.74
9C
H3O
H13
0−12
062
5.74
922
3.82
1.11
e-03
12.1
40.
033.
790.
070.
3715
1.58
0.03
625.
902
HC
l1 3
/2−
0 3/2
625.
902
30.0
41.
17e-
0313
B:H
Cl(
1 5/2−
0 3/2
)62
5.91
9H
Cl
1 5/2−
0 3/2
625.
919
30.0
41.
17e-
0315
B:H
Cl(
1 3/2−
0 3/2
)62
5.93
2H
Cl
1 1/2−
0 3/2
625.
932
30.0
41.
17e-
0314
B:H
Cl(
1 3/2−
0 3/2
)62
6.55
5C
H3O
H17
0−16
162
6.55
536
6.79
9.51
e-04
15B
:CH
3OH
(13 4−
124)
626.
555
CH
3OH
134−
124
626.
555
573.
971.
49e-
0315
B:C
H3O
H(1
7 0−
161)
626.
626
CH
3OH
3 2−
2 162
6.62
651
.64
1.23
e-03
11.7
00.
024.
870.
040.
4719
2.52
0.03
627.
170
CH
3OH
13−
1−12−
162
7.17
021
6.53
1.11
e-03
12.0
40.
044.
140.
090.
6415
3.24
0.03
627.
558
CH
3OH
130−
120
627.
558
211.
031.
12e-
0311
.97
0.03
4.14
0.08
0.65
143.
170.
0362
8.05
2C
H3O
H13
2−12
262
8.05
224
8.84
1.10
e-03
12.1
50.
094.
730.
210.
1315
0.64
0.03
628.
330
CH
3OH
13−
4−12−
462
8.33
029
9.06
1.51
e-03
11.7
20.
062.
690.
140.
0513
0.40
0.02
628.
409
CH
3OH
134−
124
628.
409
307.
181.
02e-
0312
.42
0.46
3.89
1.07
0.02
140.
100.
0262
8.44
5C
H3O
H13−
3−12−
362
8.44
527
3.90
1.59
e-03
14B
:CH
3OH
(13 3−
123)
628.
470
CH
3OH
133−
123
628.
470
260.
991.
06e-
0313
B:C
H3O
H(1
3 −3−
12−
3)62
8.47
0C
H3O
H13
3−12
362
8.47
026
0.99
1.58
e-03
14B
:CH
3OH
(13 −
3−12−
3)62
8.51
2C
H3O
H13
4−12
462
8.51
229
1.53
1.51
e-03
14B
:CH
3OH
(13 4−
124)
628.
513
CH
3OH
134−
124
628.
513
291.
531.
51e-
0313
B:C
H3O
H(1
3 4−
124)
628.
525
CH
3OH
133−
123
628.
525
261.
001.
58e-
0313
B:C
H3O
H(1
3 4−
124)
628.
696
CH
3OH
131−
121
628.
696
232.
291.
14e-
0312
.12
0.03
4.12
0.06
0.24
141.
150.
0262
8.81
6C
H3O
H13
3−12
362
8.81
625
8.96
1.07
e-03
12.3
90.
176.
480.
410.
0813
0.46
0.02
628.
869
CH
3OH
132−
122
628.
869
248.
981.
11e-
0312
.04
0.11
4.66
0.25
0.12
140.
620.
0262
9.14
0C
H3O
H3 2−
2 162
9.14
051
.64
1.25
e-03
11.7
30.
054.
260.
110.
4817
2.35
0.03
629.
322
CH
3OH
132−
122
629.
322
233.
611.
09e-
0312
.05
0.05
4.25
0.12
0.34
171.
680.
0362
9.65
2C
H3O
H13−
2−12−
262
9.65
223
7.30
1.11
e-03
12.2
00.
034.
840.
070.
1716
0.90
0.02
629.
921
CH
3OH
7 1−
6 062
9.92
178
.97
7.78
e-04
12.0
20.
024.
180.
041.
0216
4.96
0.03
631.
703
H2C
O9 1
,9−
8 1,8
631.
703
163.
607.
46e-
0311
.95
0.02
4.86
0.04
0.86
444.
960.
0863
3.42
3C
H3O
H13
1−12
163
3.42
322
7.48
1.15
e-03
12.2
90.
043.
680.
100.
3443
1.66
0.07
634.
511
HN
C7 0
,0−
6 0,0
634.
511
121.
821.
29e-
0211
.66
0.06
2.95
0.15
0.11
330.
420.
0563
6.19
3C
H3O
H16
4−16
363
6.19
339
5.93
2.23
e-03
31B
:CH
3OH
(13 4−
133)
636.
197
CH
3OH
134−
133
636.
197
291.
532.
14e-
0332
B:C
H3O
H(1
6 4−
163)
636.
199
CH
3OH
174−
173
636.
199
435.
372.
25e-
0331
B:C
H3O
H(1
6 4−
163)
636.
274
CH
3OH
9 4−
9 363
6.27
418
4.79
1.95
e-03
35B
:CH
3OH
(10 4−
103)
636.
279
CH
3OH
104−
103
636.
279
207.
992.
02e-
0331
B:C
H3O
H(9
4−9 3
)63
6.28
1C
H3O
H11
4−11
363
6.28
123
3.52
2.07
e-03
30B
:CH
3OH
(94−
9 3)
636.
291
CH
3OH
9 4−
9 363
6.29
118
4.79
1.96
e-03
31B
:CH
3OH
(94−
9 3)
636.
299
CH
3OH
124−
123
636.
299
261.
362.
11e-
0332
B:C
H3O
H(9
4−9 3
)
A57, page 25 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
636.
303
CH
3OH
8 4−
8 363
6.30
316
3.90
1.87
e-03
31B
:CH
3OH
(94−
9 3)
636.
312
CH
3OH
8 4−
8 363
6.31
216
3.90
1.87
e-03
31B
:CH
3OH
(94−
9 3)
636.
334
CH
3OH
7 4−
7 363
6.33
414
5.33
1.76
e-03
27B
:CH
3OH
(84−
8 3)
636.
337
CH
3OH
7 4−
7 363
6.33
714
5.33
1.76
e-03
33B
:CH
3OH
(84−
8 3)
636.
364
CH
3OH
6 4−
6 363
6.36
412
9.09
1.60
e-03
37B
:CH
3OH
(64−
6 3)
636.
366
CH
3OH
6 4−
6 363
6.36
612
9.09
1.60
e-03
37B
:CH
3OH
(74−
7 3)
636.
393
CH
3OH
5 4−
5 363
6.39
311
5.16
1.34
e-03
31B
:CH
3OH
(64−
6 3)
636.
394
CH
3OH
5 4−
5 363
6.39
411
5.16
1.34
e-03
34B
:CH
3OH
(64−
6 3)
636.
523
CH
3OH
154−
153
636.
523
358.
812.
21e-
0335
B:C
S(1
3−12
)63
6.53
2C
S13−
1263
6.53
221
3.90
5.56
e-03
35B
:CH
3OH
(15 4−
153)
638.
280
CH
3OH
100−
9 −1
638.
280
140.
608.
35e-
0412
.26
0.06
3.96
0.13
0.46
422.
050.
0763
8.52
4C
H3O
H8 3−
7 263
8.52
413
3.36
1.13
e-03
11.9
70.
053.
930.
120.
5141
2.45
0.06
638.
818
CH
3OH
8 3−
7 263
8.81
813
3.36
1.13
e-03
11.9
80.
063.
910.
140.
5735
2.80
0.06
645.
254
SO15
15−
1414
645.
254
260.
943.
62e-
0311
.61
0.09
9.64
0.20
0.05
360.
360.
0664
5.87
5SO
1516−
1415
645.
875
252.
603.
65e-
038.
790.
086.
640.
180.
0934
0.43
0.06
647.
082
H2C
O9 0
,9−
8 0,8
647.
082
156.
188.
10e-
0311
.80
0.02
4.91
0.05
0.55
283.
100.
0564
9.54
0C
H3O
H14
1−13
264
9.54
026
4.78
5.20
e-04
27B
:CH
3OH
(14 1−
132)
649.
540
CH
3OH
141−
132
649.
540
264.
787.
71e-
0426
B:C
H3O
H(1
4 1−
132)
651.
617
CH
3OH
101−
9 065
1.61
714
8.73
7.51
e-04
11.8
70.
034.
460.
060.
3725
1.93
0.04
652.
096
N2H
+7−
665
2.09
612
5.19
1.87
e-02
11.4
90.
022.
240.
051.
8030
5.79
0.05
653.
970
H2C
O9 2
,8−
8 2,7
653.
970
204.
237.
96e-
0311
.95
0.03
3.88
0.07
0.30
311.
580.
0565
4.46
3H
2CO
9 7,3−
8 7,2
654.
463
732.
273.
32e-
0332
B:H
2CO
(97,
2−8 7
,1)
654.
463
H2C
O9 7
,2−
8 7,1
654.
463
732.
273.
32e-
0332
B:H
2CO
(97,
3−8 7
,2)
655.
212
H2C
O9 5
,5−
8 5,4
655.
212
451.
245.
83e-
0331
B:H
2CO
(95,
4−8 5
,3)
655.
212
H2C
O9 5
,4−
8 5,3
655.
212
451.
245.
83e-
0330
B:H
2CO
(95,
5−8 5
,4)
655.
640
H2C
O9 4
,6−
8 4,5
655.
640
345.
606.
77e-
0328
B:H
2CO
(94,
5−8 4
,4)
655.
644
H2C
O9 4
,5−
8 4,4
655.
644
345.
606.
77e-
0328
B:H
2CO
(94,
6−8 4
,5)
656.
165
H2C
O9 3
,7−
8 3,6
656.
165
263.
377.
52e-
0330
B:C
H3O
H(1
3 2−
121)
656.
169
CH
3OH
132−
121
656.
169
233.
617.
87e-
0430
B:H
2CO
(93,
7−8 3
,6)
656.
465
H2C
O9 3
,6−
8 3,5
656.
465
263.
407.
53e-
0311
.85
0.02
4.78
0.05
0.44
292.
340.
0565
8.55
3C
18O
6−5
658.
553
110.
631.
86e-
0511
.39
0.02
2.22
0.04
0.93
273.
460.
0566
1.06
713
CO
6−5
661.
067
111.
051.
88e-
0511
.54
0.01
3.22
0.04
6.18
2828
.65
0.06
662.
209
H2C
O9 2
,7−
8 2,6
662.
209
205.
338.
27e-
0312
.09
0.04
5.29
0.10
0.23
261.
390.
0566
5.44
2C
H3O
H5 −
2−4 −
166
5.44
260
.73
1.27
e-03
12.0
00.
024.
910.
050.
6730
3.66
0.04
668.
117
CH
3OH
180−
171
668.
117
408.
237.
64e-
0412
.54
0.30
3.67
0.71
0.06
250.
250.
0467
0.42
3C
H3O
H14
1−13
167
0.42
325
6.02
1.36
e-03
12.0
40.
034.
710.
060.
2429
1.35
0.05
672.
903
CH
3OH
17−
1−16
067
2.90
335
9.92
1.53
e-03
12.1
00.
074.
250.
170.
2629
1.32
0.04
673.
416
CH
3OH
140−
130
673.
416
256.
141.
38e-
0312
.32
0.08
4.69
0.18
0.29
281.
520.
0467
3.74
6C
H3O
H4 2−
3 167
3.74
660
.92
1.34
e-03
11.7
00.
024.
620.
040.
5430
2.91
0.05
674.
009
C17
O6 7
/2−
5 9/2
674.
009
113.
238.
37e-
0832
B:C
H3O
H(1
4 1−
131)
674.
017
CH
3OH
141−
131
674.
017
568.
002.
06e-
0332
B:C
17O
(67/
2−5 9
/2)
674.
791
CH
3OH
142−
132
674.
791
541.
672.
02e-
0331
B:H
2CO
(91,
8−8 1
,7)
674.
810
H2C
O9 1
,8−
8 1,7
674.
810
173.
999.
09e-
0332
B:C
H3O
H(1
4 2−
132)
A57, page 26 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
674.
991
CH
3OH
8 1−
7 067
4.99
197
.38
9.56
e-04
12.0
90.
024.
690.
041.
0633
5.55
0.06
675.
135
CH
3OH
14−
1−13−
167
5.13
524
8.94
1.39
e-03
12.1
30.
024.
250.
050.
5731
2.97
0.05
675.
613
CH
3OH
140−
130
675.
613
243.
451.
40e-
0312
.23
0.04
4.23
0.09
0.61
293.
070.
0567
5.77
3C
H3O
H3 3−
2 267
5.77
361
.64
2.56
e-03
12.3
50.
085.
220.
200.
4433
1.54
0.06
676.
215
CH
3OH
142−
132
676.
215
281.
291.
38e-
0312
.08
0.06
6.04
0.15
0.11
310.
650.
0567
6.49
5C
H3O
H14
5−13
567
6.49
537
9.68
1.23
e-03
32B
:CH
3OH
(19 0−
181)
676.
499
CH
3OH
190−
181
676.
499
440.
099.
84e-
0434
B:C
H3O
H(1
4 5−
135)
676.
585
CH
3OH
14−
4−13−
467
6.58
533
1.54
1.29
e-03
12.4
20.
084.
240.
180.
0731
0.40
0.04
676.
749
CH
3OH
143−
133
676.
749
293.
471.
34e-
0312
.17
0.06
4.18
0.14
0.12
280.
480.
0467
6.82
2C
H3O
H14
4−13
467
6.82
232
4.01
1.30
e-03
31B
:CH
3OH
(14 4−
134)
676.
824
CH
3OH
144−
134
676.
824
324.
011.
30e-
0331
B:C
H3O
H(1
4 4−
134)
676.
830
CH
3OH
143−
133
676.
830
293.
481.
34e-
0330
B:C
H3O
H(1
4 4−
134)
677.
013
CH
3OH
141−
131
677.
013
264.
781.
43e-
0312
.19
0.04
4.25
0.09
0.20
310.
930.
0567
7.19
1C
H3O
H14
3−13
367
7.19
129
1.46
1.35
e-03
29B
:CH
3OH
(14 2−
132)
677.
233
CH
3OH
142−
132
677.
233
281.
491.
39e-
0326
B:C
H3O
H(1
4 3−
133)
677.
710
CH
3OH
142−
132
677.
710
266.
141.
37e-
0312
.17
0.03
4.09
0.06
0.32
461.
530.
0767
8.25
3C
H3O
H14−
2−13−
267
8.25
326
9.85
1.39
e-03
12.0
90.
056.
150.
110.
2029
1.13
0.04
678.
785
CH
3OH
4 2−
3 167
8.78
560
.93
1.37
e-03
11.9
00.
024.
520.
050.
5827
2.78
0.03
680.
047
CN
6 11/
2,13/2−
5 9/2,1
1/2
680.
047
114.
233.
50e-
0331
B:C
N(6
11/2,9/2−
5 9/2,7/2
)68
0.04
7C
N6 1
1/2,
9/2−
5 9/2,7/2
680.
047
114.
223.
36e-
0331
B:C
N(6
11/2,1
3/2−
5 9/2,1
1/2)
680.
047
CN
6 11/
2,11/2−
5 9/2,9/2
680.
047
114.
223.
38e-
0331
B:C
N(6
11/2,1
3/2−
5 9/2,1
1/2)
680.
264
CN
6 13/
2,13/2−
5 11/
2,11/2
680.
264
114.
293.
47e-
0331
B:C
N(6
13/2,1
5/2−
5 11/
2,13/2
)68
0.26
4C
N6 1
3/2,
15/2−
5 11/
2,13/2
680.
264
114.
293.
56e-
0330
B:C
N(6
13/2,1
3/2−
5 11/
2,11/2
)68
0.26
4C
N6 1
3/2,
11/2−
5 11/
2,9/
268
0.26
411
4.29
3.46
e-03
31B
:CN
(613/2,1
3/2−
5 11/
2,11/2
)68
1.99
0C
H3O
H14
1−13
168
1.99
026
0.21
1.43
e-03
12.3
20.
034.
860.
070.
3829
2.06
0.04
685.
435
CS
14−
1368
5.43
524
6.79
6.96
e-03
31B
:CH
3OH
(11 0−
10−
1)68
5.50
5C
H3O
H11
0−10−
168
5.50
516
6.05
1.10
e-03
29B
:CS
(14−
13)
686.
732
CH
3OH
9 3−
8 268
6.73
215
4.25
1.34
e-03
12.1
00.
024.
160.
050.
5130
2.44
0.05
687.
225
CH
3OH
9 3−
8 268
7.22
515
4.25
1.34
e-03
11.8
30.
024.
450.
050.
5031
2.42
0.05
687.
303
H2S
2 0,2−
1 1,1
687.
303
54.7
09.
32e-
0411
.64
0.03
3.82
0.06
0.34
361.
590.
0569
1.47
3C
O6−
569
1.47
311
6.16
2.14
e-05
11.3
00.
0313
.00
0.07
19.5
031
204.
500.
1069
7.14
6C
H3O
H15
1−14
269
7.14
629
9.59
6.56
e-04
11.3
70.
071.
860.
150.
1237
0.25
0.05
698.
545
CC
H8 1
7/2,
8−7 1
5/2,
769
8.54
515
0.88
1.10
e-03
33B
:CC
H(8
17/2,9−
7 15/
2,8)
698.
545
CC
H8 1
7/2,
9−7 1
5/2,
869
8.54
515
0.88
1.11
e-03
31B
:CC
H(8
17/2,8−
7 15/
2,7)
698.
607
CC
H8 1
5/2,
8−7 1
3/2,
769
8.60
715
0.91
1.10
e-03
34B
:CC
H(8
17/2,8−
7 15/
2,7)
698.
607
CC
H8 1
5/2,
7−7 1
3/2,
669
8.60
715
0.91
1.09
e-03
33B
:CC
H(8
17/2,8−
7 15/
2,7)
701.
367
CH
3OH
111−
100
701.
367
174.
279.
33e-
0429
B:H
2CO
(10 1
,10−
9 1,9
)70
1.37
0H
2CO
101,
10−
9 1,9
701.
370
197.
261.
03e-
0231
B:C
H3O
H(1
1 1−
100)
705.
182
CH
3OH
142−
131
705.
182
266.
149.
56e-
0412
.09
0.04
4.56
0.09
0.23
331.
180.
0570
8.87
7H
CN
8−7
708.
877
153.
111.
74e-
0212
.37
0.04
11.0
10.
091.
6742
18.7
50.
0971
3.34
1H
CO
+8−
771
3.34
115
4.07
3.02
e-02
11.3
50.
014.
790.
032.
7933
16.6
90.
0871
3.98
2C
H3O
H6 −
2−5 −
171
3.98
274
.66
1.45
e-03
11.8
50.
024.
810.
050.
5639
2.92
0.06
716.
938
H2C
O10
0,10−
9 0,9
716.
938
190.
581.
11e-
0211
.97
0.05
3.99
0.12
0.29
481.
380.
0771
8.15
9C
H3O
H15
1−14
171
8.15
929
0.49
1.68
e-03
12.4
60.
064.
350.
140.
1543
0.78
0.06
A57, page 27 of 36
A&A 556, A57 (2013)
Tabl
eA
.1.c
ontin
ued.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
Tm
brm
sFl
uxδF
lux
Ble
nd(B
)/N
otes
GH
zG
Hz
Kra
d/s
kms−
1km
s−1
kms−
1km
s−1
Km
KK
kms−
1K
kms−
1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
718.
436
CH
3OH
4 −4−
3 −3
718.
436
111.
123.
06e-
0311
.75
0.03
4.56
0.07
0.38
401.
900.
0671
9.66
5C
H3O
H9 1−
8 071
9.66
511
8.08
1.16
e-03
12.1
70.
024.
460.
041.
0427
5.38
0.05
720.
441
CH
3OH
5 2−
4 172
0.44
172
.53
1.50
e-03
11.9
20.
024.
900.
060.
6032
3.49
0.06
721.
011
CH
3OH
150−
140
721.
011
290.
741.
70e-
0312
.60
0.03
4.61
0.07
0.25
261.
230.
0472
3.04
0C
H3O
H15−
1−14−
172
3.04
028
3.64
1.71
e-03
12.2
10.
024.
250.
050.
5028
2.50
0.04
723.
280
CH
3OH
18−
1−17
072
3.28
040
1.50
1.98
e-03
12.4
80.
045.
370.
090.
2030
1.08
0.05
723.
619
CH
3OH
150−
140
723.
619
278.
181.
72e-
0312
.13
0.02
4.27
0.04
0.56
312.
520.
0572
4.12
2C
H3O
H4 3−
3 272
4.12
270
.93
2.56
e-03
12.2
60.
025.
380.
050.
4831
2.77
0.05
724.
345
CH
3OH
152−
142
724.
345
316.
051.
71e-
0312
.26
0.07
5.00
0.16
0.10
340.
510.
0572
5.01
3C
H3O
H15
3−14
372
5.01
332
8.26
2.47
e-03
12.6
70.
135.
120.
300.
0834
0.36
0.05
725.
122
CH
3OH
154−
144
725.
122
358.
812.
39e-
0331
B:C
H3O
H(1
5 4−
144)
725.
126
CH
3OH
154−
144
725.
126
358.
812.
39e-
0331
B:C
H3O
H(1
5 4−
144)
725.
126
CH
3OH
153−
143
725.
126
328.
282.
47e-
0331
B:C
H3O
H(1
5 4−
144)
725.
316
CH
3OH
151−
141
725.
316
299.
591.
76e-
0312
.15
0.08
3.98
0.20
0.18
320.
720.
0572
5.56
5C
H3O
H15
3−14
372
5.56
532
6.28
2.48
e-03
24B
:CH
3OH
(15 2−
142)
725.
594
CH
3OH
152−
142
725.
594
316.
311.
72e-
0326
B:C
H3O
H(1
5 3−
143)
726.
052
CH
3OH
152−
142
726.
052
300.
981.
70e-
0312
.47
0.03
4.62
0.08
0.30
281.
530.
0472
6.20
8H
2CO
102,
9−9 2
,872
6.20
823
9.08
1.11
e-02
12.2
30.
045.
160.
100.
1729
0.86
0.04
726.
899
CH
3OH
15−
2−14−
272
6.89
930
4.74
1.72
e-03
12.1
10.
164.
340.
380.
1332
0.44
0.05
728.
054
H2C
O10
5,6−
9 5,5
728.
054
486.
188.
72e-
0325
B:H
2CO
(10 5
,5−
9 5,4
)72
8.05
4H
2CO
105,
5−9 5
,472
8.05
448
6.18
8.72
e-03
26B
:H2C
O(1
0 5,6−
9 5,5
)72
8.58
3H
2CO
104,
7−9 4
,672
8.58
338
0.57
9.78
e-03
25B
:H2C
O(1
0 4,6−
9 4,5
)72
8.59
2H
2CO
104,
6−9 4
,572
8.59
238
0.57
9.78
e-03
25B
:H2C
O(1
0 4,7−
9 4,6
)72
8.86
2C
H3O
H5 2−
4 172
8.86
272
.53
1.55
e-03
11.8
20.
024.
850.
040.
6328
3.20
0.05
729.
213
H2C
O10
3,8−
9 3,7
729.
213
298.
361.
06e-
0212
.14
0.02
5.10
0.06
0.29
241.
480.
0472
9.72
5H
2CO
103,
7−9 3
,672
9.72
529
8.42
1.06
e-02
12.0
50.
024.
210.
050.
3225
1.56
0.04
730.
520
CH
3OH
151−
141
730.
520
295.
271.
77e-
0328
B:C
H3O
H(2
0 0−
191)
730.
550
CH
3OH
200−
191
730.
550
486.
301.
26e-
0326
B:C
H3O
H(1
5 1−
141)
731.
596
SO17
18−
1617
731.
596
320.
775.
32e-
038.
980.
108.
660.
230.
0524
0.33
0.04
732.
432
CH
3OH
120−
11−
173
2.43
219
3.79
1.42
e-03
12.2
10.
024.
380.
050.
4428
2.33
0.04
734.
324
CS
15−
1473
4.32
428
2.04
8.58
e-03
12.2
10.
1511
.05
0.35
0.17
261.
900.
0573
4.89
4C
H3O
H10
3−9 2
734.
894
177.
461.
58e-
0311
.88
0.06
5.03
0.14
0.46
252.
500.
0473
5.67
3C
H3O
H10
3−9 2
735.
673
177.
461.
58e-
0312
.06
0.05
4.47
0.11
0.46
252.
220.
0473
6.03
4H
2S2 1
,2−
1 0,1
736.
034
55.1
01.
33e-
0311
.65
0.07
5.27
0.16
0.92
295.
300.
0673
7.34
3H
2CO
102,
8−9 2
,773
7.34
324
0.72
1.16
e-02
11.8
40.
044.
940.
100.
1926
1.01
0.04
745.
210
N2H
+8−
774
5.21
016
0.96
2.81
e-02
11.5
10.
022.
600.
061.
1832
4.09
0.05
749.
072
H2C
O10
1,9−
9 1,8
749.
072
209.
941.
25e-
0212
.06
0.02
5.59
0.04
0.59
363.
490.
0675
1.55
1C
H3O
H12
1−11
075
1.55
120
2.12
1.14
e-03
12.1
60.
034.
380.
070.
3535
1.61
0.06
752.
033
H2O
2 1,1,0−
2 0,2,0
752.
033
136.
946.
98e-
0311
.91
0.06
14.8
80.
142.
1943
38.5
10.
1575
2.31
2C
H3O
H7 −
5−7 −
475
2.31
218
9.00
2.35
e-03
12.2
30.
117.
290.
250.
0641
0.37
0.05
754.
222
CH
3OH
152−
141
754.
222
300.
981.
15e-
0312
.14
0.04
3.83
0.11
0.21
361.
020.
0676
2.63
6C
H3O
H7 −
2−6 −
176
2.63
690
.91
1.66
e-03
12.0
40.
024.
960.
040.
6038
2.99
0.06
762.
676
CH
3OH
13−
3−13−
276
2.67
627
3.90
2.31
e-03
12.0
30.
294.
790.
690.
0739
0.31
0.04
763.
883
CH
3OH
12−
3−12−
276
3.88
324
3.74
2.32
e-03
12.6
70.
082.
800.
190.
1133
0.44
0.04
763.
951
CH
3OH
8 5−
9 476
3.95
122
1.45
4.87
e-04
38B
:CH
3OH
(85−
9 4)
A57, page 28 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
763.
951
CH
3OH
8 5−
9 476
3.95
122
1.45
4.87
e-04
40B
:CH
3OH
(85−
9 4)
763.
953
CH
3OH
101−
9 076
3.95
314
1.08
1.39
e-03
40B
:CH
3OH
(85−
9 4)
764.
812
CH
3OH
11−
3−11−
276
4.81
221
5.90
2.31
e-03
12.0
20.
074.
950.
160.
1337
0.59
0.05
765.
513
CH
3OH
10−
3−10−
276
5.51
319
0.37
2.30
e-03
12.3
10.
0810
.55
0.18
0.12
340.
950.
0676
5.86
6C
H3O
H16
1−15
176
5.86
632
7.24
2.04
e-03
12.5
40.
055.
190.
120.
1542
0.87
0.06
766.
028
CH
3OH
9 −3−
9 −2
766.
028
167.
162.
28e-
0312
.19
0.06
5.33
0.15
0.18
380.
840.
0576
6.39
6C
H3O
H8 −
3−8 −
276
6.39
614
6.28
2.24
e-03
12.1
10.
056.
610.
120.
1942
1.16
0.07
766.
648
CH
3OH
7 −3−
7 −2
766.
648
127.
712.
18e-
0312
.28
0.05
5.61
0.13
0.21
391.
240.
0576
6.71
0C
H3O
H6 2−
5 176
6.71
086
.46
1.69
e-03
11.9
40.
034.
750.
060.
5942
2.69
0.06
766.
761
CH
3OH
5 −4−
4 −3
766.
761
122.
723.
13e-
0311
.67
0.03
3.99
0.07
0.43
421.
920.
0676
6.81
0C
H3O
H6 −
3−6 −
276
6.81
011
1.46
2.10
e-03
11.9
70.
045.
320.
100.
2045
1.03
0.06
766.
908
CH
3OH
5 −3−
5 −2
766.
908
97.5
31.
96e-
0311
.89
0.04
3.00
0.10
0.24
430.
750.
0576
6.96
0C
H3O
H4 −
3−4 −
276
6.96
085
.92
2.54
e-03
39B
:CH
3OH
(3−
3−3 −
2)76
6.98
2C
H3O
H3 −
3−3 −
276
6.98
276
.64
1.81
e-03
38B
:CH
3OH
(4−
3−4 −
2)76
8.25
2C
18O
7−6
768.
252
147.
502.
98e-
0511
.31
0.03
3.19
0.06
0.56
462.
510.
0776
8.54
0C
H3O
H16
0−15
076
8.54
032
7.63
2.06
e-03
12.3
10.
045.
030.
100.
2044
1.09
0.06
770.
886
CH
3OH
16−
1−15−
177
0.88
632
0.63
3.08
e-03
36B
:H2C
O(1
1 1,1
1−10
1,10
)77
0.89
6H
2CO
111,
11−
101,
1077
0.89
623
4.26
1.37
e-02
36B
:CH
3OH
(16 −
1−15−
1)77
1.18
413
CO
7−6
771.
184
148.
063.
01e-
0511
.37
0.02
3.58
0.04
4.91
3623
.54
0.07
771.
576
CH
3OH
160−
150
771.
576
315.
212.
10e-
0312
.32
0.02
4.08
0.05
0.46
352.
060.
0577
2.45
4C
H3O
H5 3−
4 277
2.45
482
.53
2.70
e-03
12.7
40.
036.
210.
060.
5140
3.45
0.06
773.
259
CH
3OH
163−
153
773.
259
365.
372.
03e-
0311
.95
0.07
5.15
0.16
0.10
380.
400.
0577
3.41
6C
H3O
H16
3−15
377
3.41
636
5.40
3.01
e-03
11.9
70.
195.
040.
450.
1238
0.65
0.06
773.
602
CH
3OH
161−
151
773.
602
336.
722.
13e-
0312
.72
0.04
3.31
0.10
0.13
400.
500.
0677
3.89
3C
H3O
H19−
1−18
077
3.89
344
5.37
2.53
e-03
12.2
90.
065.
360.
130.
1335
0.66
0.05
773.
941
CH
3OH
163−
153
773.
941
363.
433.
03e-
0335
B:C
H3O
H(1
6 2−
152)
773.
950
CH
3OH
162−
152
773.
950
353.
453.
10e-
0335
B:C
H3O
H(1
6 3−
153)
774.
333
CH
3OH
162−
152
774.
333
338.
142.
07e-
0312
.01
0.04
3.24
0.10
0.21
390.
710.
0677
5.59
6C
H3O
H16−
2−15−
277
5.59
634
1.96
2.10
e-03
11.7
40.
093.
820.
200.
1141
0.39
0.06
779.
009
CH
3OH
161−
151
779.
009
332.
652.
15e-
0340
B:C
H3O
H(1
3 0−
12−
1)77
9.03
1C
H3O
H13
0−12−
177
9.03
122
3.82
1.82
e-03
40B
:CH
3OH
(16 1−
151)
779.
380
CH
3OH
6 2−
5 177
9.38
086
.46
1.78
e-03
11.8
50.
025.
080.
060.
5541
2.60
0.07
780.
039
H237
Cl+
2 1,2,5/2−
1 0,1,5/2
780.
039
57.6
61.
78e-
039.
381.
091.
151.
52−
0.07
35-0
.38
0.04
781.
609
H2C
l+2 1
,2,5/2−
1 0,1,5/2
781.
609
57.7
51.
79e-
0332
B:H
2Cl+
(21,
2,7/
2−1 0
,1,5/2
)78
1.62
2H
2Cl+
2 1,2,5/2−
1 0,1,3/2
781.
622
57.7
54.
17e-
0330
B:H
2Cl+
(21,
2,7/
2−1 0
,1,5/2
)78
1.62
7H
2Cl+
2 1,2,7/2−
1 0,1,5/2
781.
627
57.7
55.
96e-
0331
B:H
2Cl+
(21,
2,5/
2−1 0
,1,5/2
)78
1.62
8H
2Cl+
2 1,2,1/2−
1 0,1,1/2
781.
628
57.7
54.
96e-
0330
B:H
2Cl+
(21,
2,5/
2−1 0
,1,5/2
)78
3.00
2C
H3O
H11
3−10
278
3.00
220
2.98
1.85
e-03
12.0
80.
034.
390.
070.
4333
2.13
0.05
783.
199
CS
16−
1578
3.19
931
9.62
1.04
e-02
12.8
00.
2710
.51
0.62
0.13
321.
270.
0578
4.17
7C
H3O
H11
3−10
278
4.17
720
2.99
1.86
e-03
12.1
60.
034.
210.
060.
4135
1.89
0.05
784.
693
CH
3OH
210−
201
784.
693
534.
791.
60e-
0312
.66
0.05
3.86
0.12
0.14
300.
610.
0478
5.80
2C
CH
9 19/
2,9−
8 17/
2,8
785.
802
188.
591.
58e-
0335
B:C
CH
(919/2,1
0−8 1
7/2,
9)78
5.80
2C
CH
9 19/
2,10−
8 17/
2,9
785.
802
188.
591.
59e-
0335
B:C
CH
(919/2,9−
8 17/
2,8)
786.
280
C17
O7 9
/2−
6 11/
278
6.28
015
0.96
6.36
e-08
39B
:H2C
O(1
1 0,1
1−10
0,10
)
A57, page 29 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
786.
285
H2C
O11
0,11−
100,
1078
6.28
522
8.32
1.47
e-02
39B
:C17
O(7
9/2−
6 11/
2)79
3.33
6C
N7 1
3/2,
15/2−
6 11/
2,13/2
793.
336
152.
305.
64e-
0335
B:C
N(7
13/2,1
1/2−
6 11/
2,9/
2)79
3.33
6C
N7 1
3/2,
11/2−
6 11/
2,9/
279
3.33
615
2.30
5.48
e-03
35B
:CN
(713/2,1
5/2−
6 11/
2,13/2
)79
3.33
7C
N7 1
3/2,
13/2−
6 11/
2,11/2
793.
337
152.
305.
51e-
0335
B:C
N(7
13/2,1
5/2−
6 11/
2,13/2
)79
3.55
3C
N7 1
5/2,
15/2−
6 13/
2,13/2
793.
553
152.
385.
61e-
0336
B:C
N(7
15/2,1
7/2−
6 13/
2,15/2
)79
3.55
3C
N7 1
5/2,
17/2−
6 13/
2,15/2
793.
553
152.
385.
71e-
0337
B:C
N(7
15/2,1
5/2−
6 13/
2,13/2
)79
3.55
4C
N7 1
5/2,
13/2−
6 13/
2,11/2
793.
554
152.
385.
59e-
0335
B:C
N(7
15/2,1
5/2−
6 13/
2,13/2
)79
7.43
3H
CN
9−8
797.
433
191.
382.
49e-
0212
.44
0.02
11.9
30.
041.
1447
14.6
00.
1179
8.31
3H
2CO
112,
10−
102,
979
8.31
327
7.39
1.49
e-02
9.62
0.30
6.16
0.71
0.10
490.
490.
0780
2.24
1C
H3O
H13
1−12
080
2.24
123
2.29
1.38
e-03
12.3
10.
072.
470.
160.
2058
0.52
0.07
802.
282
H2C
O11
3,9−
103,
880
2.28
233
6.87
1.45
e-02
11.8
20.
073.
200.
170.
1957
0.51
0.07
802.
458
HC
O+
9−8
802.
458
192.
594.
33e-
0211
.55
0.02
5.42
0.04
2.00
5713
.19
0.12
803.
112
H2C
O11
3,8−
103,
780
3.11
233
6.96
1.45
e-02
12.2
70.
073.
640.
170.
1959
0.77
0.08
803.
239
CH
3OH
162−
151
803.
239
338.
141.
38e-
0312
.25
0.08
5.16
0.18
0.14
560.
570.
0880
6.65
2C
O7−
680
6.65
215
4.88
3.42
e-05
11.2
70.
0313
.27
0.06
20.4
249
211.
460.
1480
7.86
6C
H3O
H11
1−10
080
7.86
616
6.37
1.65
e-03
51B
:CH
3OH
(11 1−
100)
807.
866
CH
3OH
111−
100
807.
866
166.
371.
65e-
0350
B:C
H3O
H(1
1 1−
100)
809.
342
C2−
180
9.34
262
.46
2.67
e-07
11.9
80.
021.
800.
051.
4747
4.90
0.07
811.
445
CH
3OH
8 −2−
7 −1
811.
445
109.
491.
88e-
0312
.38
0.03
5.11
0.06
0.57
492.
980.
0781
2.55
0C
H3O
H7 2−
6 181
2.55
010
2.70
1.92
e-03
12.1
60.
035.
050.
060.
5443
2.70
0.06
812.
831
H2C
O11
2,9−
102,
881
2.83
127
9.73
1.57
e-02
11.9
30.
108.
710.
240.
0941
0.77
0.06
813.
542
CH
3OH
171−
161
813.
542
366.
292.
45e-
0313
.96
0.33
8.69
0.82
0.14
430.
990.
0681
5.07
1C
H3O
H6 −
4−5 −
381
5.07
113
6.65
3.31
e-03
11.9
10.
024.
390.
060.
4341
1.76
0.06
816.
011
CH
3OH
170−
160
816.
011
366.
792.
48e-
0312
.10
0.06
5.39
0.13
0.18
461.
200.
0781
8.66
9C
H3O
H17−
1−16−
181
8.66
935
9.92
2.50
e-03
12.6
70.
044.
150.
100.
3051
1.28
0.07
819.
479
CH
3OH
170−
160
819.
479
354.
542.
51e-
0312
.39
0.04
4.04
0.08
0.33
531.
470.
0782
0.49
9C
H3O
H17
2−16
282
0.49
939
2.50
3.71
e-03
12.1
20.
9312
.87
2.41
0.10
500.
590.
0682
0.76
2C
H3O
H6 3−
5 282
0.76
296
.46
2.93
e-03
12.1
70.
025.
180.
050.
4552
2.31
0.07
821.
698
CH
3OH
173−
163
821.
698
404.
833.
64e-
0312
.77
0.05
3.44
0.12
0.14
430.
440.
0682
1.86
9C
H3O
H17
1−16
182
1.86
937
6.17
2.56
e-03
12.4
40.
053.
750.
130.
1545
0.50
0.06
822.
301
CH
3OH
172−
162
822.
301
392.
923.
73e-
0312
.31
0.22
3.45
0.53
0.06
450.
250.
0482
2.54
0C
H3O
H17
2−16
282
2.54
037
7.62
2.49
e-03
12.2
90.
064.
450.
140.
1646
0.59
0.06
823.
083
H2C
O11
1,10−
101,
982
3.08
324
9.44
1.67
e-02
12.0
80.
034.
320.
060.
4142
1.94
0.06
824.
343
CH
3OH
17−
2−16−
282
4.34
338
1.52
2.53
e-03
12.7
30.
062.
850.
140.
1441
0.44
0.05
825.
276
CH
3OH
140−
13−
182
5.27
625
6.14
2.28
e-03
12.1
70.
044.
450.
090.
3141
1.56
0.05
827.
454
CH
3OH
171−
161
827.
454
372.
372.
58e-
0312
.68
0.06
5.47
0.14
0.19
531.
110.
0782
9.89
1C
H3O
H4 4−
3 382
9.89
110
3.56
7.63
e-03
50B
:CH
3OH
(44−
3 3)
829.
891
CH
3OH
4 4−
3 382
9.89
110
3.56
7.63
e-03
50B
:CH
3OH
(44−
3 3)
830.
349
CH
3OH
7 2−
6 183
0.34
910
2.72
2.05
e-03
12.0
40.
025.
300.
060.
6050
3.16
0.07
831.
045
CH
3OH
123−
112
831.
045
230.
832.
14e-
0311
.99
0.04
4.97
0.09
0.36
601.
680.
0883
2.05
7C
S17−
1683
2.05
735
9.56
1.25
e-02
12.4
70.
6712
.31
1.67
0.16
561.
150.
1083
2.75
4C
H3O
H12
3−11
283
2.75
423
0.83
2.16
e-03
12.1
30.
043.
950.
090.
3348
1.11
0.06
A57, page 30 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
835.
138
CH
+1−
083
5.13
840
.08
6.36
e-03
9.46
0.08
6.04
0.20
-0.4
340
-2.8
10.
0583
8.30
7N
2H+
9−8
838.
307
201.
194.
03e-
0211
.77
0.03
2.88
0.08
0.78
402.
600.
0683
8.90
2C
H3O
H22
0−21
183
8.90
258
5.57
1.99
e-03
13.4
40.
075.
050.
160.
0939
0.39
0.05
840.
276
H2C
O12
1,12−
111,
1184
0.27
627
4.58
1.79
e-02
12.1
00.
035.
220.
060.
4236
2.40
0.05
851.
415
CH
3OH
121−
110
851.
415
193.
961.
95e-
0312
.48
0.02
4.59
0.04
0.69
443.
500.
0685
2.17
7C
H3O
H17
2−16
185
2.17
737
7.62
1.65
e-03
11.8
80.
072.
850.
180.
1142
0.39
0.05
853.
504
CH
3OH
141−
130
853.
504
264.
781.
65e-
0312
.23
0.05
5.38
0.12
0.17
420.
790.
0685
7.95
9C
H3O
H8 2−
7 185
7.95
912
1.27
2.18
e-03
12.1
40.
044.
720.
080.
5757
2.83
0.07
860.
459
CH
3OH
9 −2−
8 −1
860.
459
130.
402.
13e-
0312
.20
0.03
4.89
0.06
0.53
552.
770.
0786
1.18
6C
H3O
H18
1−17
186
1.18
640
7.62
2.92
e-03
12.7
20.
429.
931.
020.
1146
0.99
0.07
863.
365
CH
3OH
7 −4−
6 −3
863.
365
152.
893.
57e-
0311
.81
0.03
5.52
0.08
0.38
472.
190.
0686
3.43
1C
H3O
H18
0−17
086
3.43
140
8.23
2.94
e-03
11.6
10.
084.
670.
190.
1447
0.58
0.05
866.
388
CH
3OH
18−
1−17−
186
6.38
840
1.50
2.97
e-03
12.9
80.
217.
750.
490.
2544
1.68
0.06
867.
327
CH
3OH
180−
170
867.
327
396.
172.
99e-
0312
.18
0.04
4.60
0.10
0.24
460.
940.
0786
9.03
8C
H3O
H7 3−
6 286
9.03
811
2.71
3.21
e-03
12.3
50.
025.
120.
060.
4554
2.26
0.08
869.
973
CH
3OH
183−
173
869.
973
446.
594.
34e-
0312
.23
0.07
5.05
0.16
0.10
520.
470.
0687
0.27
3H
2CO
122,
11−
112,
1087
0.27
331
9.16
1.94
e-02
10.9
40.
083.
730.
180.
1550
0.78
0.06
870.
664
CH
3OH
182−
172
870.
664
419.
414.
39e-
0352
B:C
H3O
H(1
8 3−
173)
870.
691
CH
3OH
183−
173
870.
691
444.
684.
36e-
0353
B:C
H3O
H(1
8 2−
172)
871.
152
CH
3OH
150−
14−
187
1.15
229
0.74
2.84
e-03
12.7
30.
034.
790.
070.
3249
1.75
0.07
873.
036
CC
H10
21/2,1
0−9 1
9/2,
987
3.03
623
0.49
2.18
e-03
38B
:CC
H(1
0 21/
2,11−
9 19/
2,10
)87
3.03
6C
CH
1021/2,1
1−9 1
9/2,
1087
3.03
623
0.49
2.19
e-03
38B
:CC
H(1
0 21/
2,10−
9 19/
2,9)
873.
138
CH
3OH
18−
2−17−
287
3.13
842
3.43
3.01
e-03
12.7
50.
068.
220.
150.
1439
0.95
0.06
873.
775
H2C
O12
5,8−
115,
787
3.77
556
6.55
1.67
e-02
34B
:H2C
O(1
2 5,7−
115,
6)87
3.77
6H
2CO
125,
7−11
5,6
873.
776
566.
551.
67e-
0235
B:H
2CO
(12 5
,8−
115,
7)87
5.36
6H
2CO
123,
10−
113,
987
5.36
637
8.88
1.91
e-02
12.2
60.
054.
080.
130.
1437
0.55
0.05
875.
735
CH
3OH
21−
1−20
087
5.73
553
9.96
3.97
e-03
12.5
80.
074.
120.
170.
0836
0.38
0.04
875.
852
CH
3OH
181−
171
875.
852
414.
403.
07e-
0312
.56
0.05
3.54
0.12
0.16
380.
560.
0587
6.64
9H
2CO
123,
9−11
3,8
876.
649
379.
031.
92e-
0212
.04
0.08
4.84
0.18
0.12
380.
680.
0587
7.92
2C
18O
8−7
877.
922
189.
644.
47e-
0511
.44
0.03
3.23
0.08
0.34
371.
380.
0587
8.22
6C
H3O
H5 4−
4 387
8.22
611
5.16
7.60
e-03
37B
:CH
3OH
(54−
4 3)
878.
227
CH
3OH
5 4−
4 387
8.22
711
5.16
7.60
e-03
40B
:CH
3OH
(54−
4 3)
879.
013
CH
3OH
133−
122
879.
013
260.
992.
48e-
0312
.19
0.04
4.77
0.08
0.23
371.
050.
0588
0.89
9C
S18−
1788
0.89
940
1.83
1.49
e-02
12.3
70.
0612
.56
1.00
0.11
391.
250.
0688
1.27
313
CO
8−7
881.
273
190.
364.
52e-
0511
.29
0.02
5.07
0.04
2.95
4215
.76
0.08
881.
421
CH
3OH
133−
122
881.
421
261.
002.
50e-
0311
.96
0.03
3.72
0.07
0.28
381.
210.
0488
1.78
2C
H3O
H8 2−
7 188
1.78
212
1.29
2.37
e-03
11.9
40.
024.
760.
060.
6335
3.28
0.05
885.
971
HC
N10−
988
5.97
123
3.90
3.44
e-02
12.5
60.
0112
.24
0.03
1.09
4014
.07
0.09
888.
629
H2C
O12
2,10−
112,
988
8.62
932
2.37
2.07
e-02
11.9
00.
427.
510.
990.
0737
0.47
0.04
891.
557
HC
O+
10−
989
1.55
723
5.38
5.97
e-02
11.4
20.
025.
520.
051.
6838
11.6
60.
0789
3.63
9H
DO
1 1,1−
0 0,0
893.
639
42.8
98.
35e-
0313
.42
0.08
2.47
0.18
0.10
370.
410.
0589
4.61
4C
H3O
H13
1−12
089
4.61
422
3.84
2.27
e-03
12.4
90.
024.
440.
050.
5736
2.76
0.06
896.
805
H2C
O12
1,11−
111,
1089
6.80
529
2.48
2.17
e-02
12.0
10.
035.
100.
080.
2933
1.75
0.05
A57, page 31 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
900.
972
CH
3OH
182−
171
900.
972
419.
411.
96e-
0311
.65
0.09
4.10
0.22
0.08
370.
370.
0590
2.93
5C
H3O
H9 2−
8 190
2.93
514
2.15
2.47
e-03
12.3
60.
025.
240.
050.
4536
2.41
0.06
905.
404
CH
3OH
151−
140
905.
404
299.
591.
94e-
0311
.90
0.06
4.81
0.14
0.17
520.
770.
0690
6.59
3C
N8 1
5/2,
17/2−
7 13/
2,15/2
906.
593
195.
818.
51e-
0353
B:C
N(8
15/2,1
3/2−
7 13/
2,11/2
)90
6.59
3C
N8 1
5/2,
13/2−
7 13/
2,11/2
906.
593
195.
818.
34e-
0353
B:C
N(8
15/2,1
7/2−
7 13/
2,15/2
)90
9.04
5O
H+
1 0,1/2−
0 1,1/2
909.
045
43.6
35.
23e-
038.
750.
213.
450.
62−
0.08
40−
0.44
0.05
909.
159
OH
+1 0
,1/2−
0 1,3/2
909.
159
43.6
31.
05e-
029.
360.
072.
740.
16−
0.20
40−
0.72
0.05
909.
508
H2C
O13
1,13−
121,
1290
9.50
831
8.23
2.28
e-02
12.1
20.
034.
330.
070.
3039
0.89
0.05
909.
738
CH
3OH
10−
2−9 −
190
9.73
815
3.63
2.38
e-03
12.3
60.
024.
970.
060.
4536
2.16
0.05
910.
808
CH
3OH
190−
180
910.
808
451.
943.
45e-
0312
.39
0.07
6.07
0.17
0.14
371.
010.
0591
1.64
2C
H3O
H8 −
4−7 −
391
1.64
217
1.46
3.89
e-03
11.8
40.
025.
290.
050.
3744
2.10
0.06
912.
109
CH
3OH
3 −3−
2 −2
912.
109
76.6
45.
85e-
0312
.18
0.02
6.01
0.05
0.45
392.
970.
0591
4.04
4C
H3O
H19−
1−18−
191
4.04
444
5.37
3.49
e-03
12.3
70.
034.
390.
080.
2338
1.06
0.05
915.
117
CH
3OH
190−
180
915.
117
440.
093.
51e-
0312
.34
0.05
4.04
0.12
0.16
430.
750.
0691
6.65
2C
H3O
H16
0−15−
191
6.65
232
7.63
3.49
e-03
12.5
20.
043.
780.
080.
2647
1.01
0.06
917.
270
CH
3OH
8 3−
7 291
7.27
013
1.28
3.53
e-03
12.6
70.
036.
110.
060.
4250
2.46
0.07
918.
699
CH
3OH
192−
182
918.
699
463.
503.
49e-
0311
.83
0.10
4.01
0.23
0.09
510.
360.
0692
1.80
0C
O8−
792
1.80
019
9.11
5.13
e-05
11.2
70.
0212
.91
0.05
23.5
648
248.
500.
1292
3.58
8H
2CO
130,
13−
120,
1292
3.58
831
3.69
2.39
e-02
12.0
20.
084.
230.
190.
1137
0.21
0.06
924.
198
CH
3OH
191−
181
924.
198
458.
763.
61e-
0312
.58
0.07
5.26
0.16
0.13
390.
630.
0592
6.55
5C
H3O
H6 4−
5 392
6.55
512
9.09
7.85
e-03
39B
:CH
3OH
(64−
5 3)
926.
555
CH
3OH
6 4−
5 392
6.55
512
9.09
7.85
e-03
40B
:CH
3OH
(64−
5 3)
926.
893
CH
3OH
143−
132
926.
893
293.
474.
20e-
0311
.38
0.04
5.90
0.10
0.25
431.
570.
0692
9.72
3C
S19−
1892
9.72
344
6.45
1.75
e-02
12.5
00.
439.
641.
020.
1245
0.95
0.08
930.
198
CH
3OH
143−
132
930.
198
293.
482.
87e-
0312
.25
0.05
4.19
0.12
0.22
440.
560.
0793
1.38
6N
2H+
10−
993
1.38
624
5.89
5.56
e-02
11.6
50.
074.
010.
170.
6245
3.03
0.06
933.
693
CH
3OH
9 2−
8 193
3.69
314
2.19
2.73
e-03
11.8
40.
035.
210.
060.
4948
2.52
0.07
937.
478
CH
3OH
141−
130
937.
478
256.
022.
64e-
0312
.46
0.02
5.78
0.05
0.48
402.
940.
0694
7.47
6C
H3O
H10
2−9 1
947.
476
165.
352.
78e-
0312
.27
0.03
4.42
0.07
0.43
611.
690.
0994
8.45
4H
2CO
133,
11−
123,
1094
8.45
442
4.40
2.46
e-02
12.2
80.
094.
270.
200.
1050
0.51
0.07
950.
365
H2C
O13
3,10−
123,
995
0.36
542
4.65
2.47
e-02
11.8
80.
184.
860.
420.
1151
0.41
0.06
959.
346
CH
3OH
11−
2−10−
195
9.34
617
9.19
2.65
e-03
13.4
20.
063.
570.
150.
3513
41.
710.
1995
9.90
1C
H3O
H9 −
4−8 −
395
9.90
119
2.34
4.26
e-03
12.8
60.
389.
231.
020.
3411
71.
500.
1796
0.47
1C
H3O
H4 −
3−3 −
296
0.47
185
.92
5.57
e-03
11.7
00.
057.
300.
110.
4411
02.
510.
1596
1.63
5C
H3O
H20−
1−19−
196
1.63
549
1.52
4.07
e-03
13.4
40.
073.
600.
160.
1474
0.50
0.08
961.
777
CH
3OH
170−
16−
196
1.77
736
6.79
4.25
e-03
12.7
10.
074.
270.
160.
2279
0.77
0.09
962.
848
CH
3OH
200−
190
962.
848
486.
304.
10e-
0311
.83
0.06
3.68
0.14
0.23
571.
140.
0796
5.44
8C
H3O
H9 3−
8 296
5.44
815
2.17
3.90
e-03
12.5
20.
035.
110.
070.
4550
2.53
0.07
966.
507
CH
3OH
203−
193
966.
507
537.
046.
00e-
0350
B:C
H3O
H(2
0 1−
191)
966.
515
CH
3OH
201−
191
966.
515
508.
386.
19e-
0352
B:C
H3O
H(2
0 3−
193)
970.
199
H2C
O13
1,12−
121,
1197
0.19
933
9.05
2.76
e-02
10.7
80.
314.
870.
720.
1482
0.67
0.11
971.
804
OH
+1 2
,5/2−
0 1,3/2
971.
804
46.6
41.
82e-
0210
8B
:OH
+(1
2,3/
2−0 1
,1/2
)97
1.80
5O
H+
1 2,3/2−
0 1,1/2
971.
805
46.6
51.
52e-
0210
7B
:OH
+(1
2,5/
2−0 1
,3/2
)
A57, page 32 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
972.
489
CH
3OH
201−
191
972.
489
505.
434.
21e-
0312
.78
0.08
2.83
0.18
0.19
990.
600.
1197
4.46
2N
H1 2
,5/2,3/2−
0 1,3/2,1/2
974.
462
46.7
75.
04e-
0355
B:N
H(1
2,3/
2,3/
2−0 1
,1/2,1/2
)97
4.47
1N
H1 2
,5/2,5/2−
0 1,3/2,3/2
974.
471
46.7
75.
66e-
0355
B:N
H(1
2,3/
2,3/
2−0 1
,1/2,1/2
)97
4.47
5N
H1 2
,3/2,3/2−
0 1,1/2,1/2
974.
475
46.7
73.
38e-
0357
B:N
H(1
2,5/
2,3/
2−0 1
,3/2,1/2
)97
4.47
8N
H1 2
,5/2,7/2−
0 1,3/2,5/2
974.
478
46.7
76.
94e-
0355
B:N
H(1
2,5/
2,3/
2−0 1
,3/2,1/2
)97
4.47
9N
H1 2
,3/2,5/2−
0 1,1/2,3/2
974.
479
46.7
86.
01e-
0356
B:N
H(1
2,5/
2,3/
2−0 1
,3/2,1/2
)97
4.48
7H
CN
11−
1097
4.48
728
0.67
4.59
e-02
55B
:NH
(12,
5/2,
3/2−
0 1,3/2,1/2
)97
4.67
3C
H3O
H15
3−14
297
4.67
332
8.26
3.24
e-03
11.5
80.
042.
140.
100.
1957
0.70
0.06
974.
877
CH
3OH
7 4−
6 397
4.87
714
5.33
8.28
e-03
56B
:CH
3OH
(74−
6 3)
974.
878
CH
3OH
7 4−
6 397
4.87
814
5.33
8.28
e-03
57B
:CH
3OH
(74−
6 3)
978.
529
CS
20−
1997
8.52
949
3.42
2.04
e-02
51B
:H2C
O(1
4 1,1
4−13
1,13
)97
8.59
2H
2CO
141,
14−
131,
1397
8.59
236
5.20
2.84
e-02
56B
:CS
(20−
19)
979.
110
CH
3OH
153−
142
979.
110
328.
283.
28e-
0312
.45
0.05
4.62
0.13
0.20
531.
080.
0798
0.02
5C
H3O
H15
1−14
098
0.02
529
0.49
3.04
e-03
12.6
80.
034.
520.
060.
4461
2.15
0.09
980.
636
HC
O+
11−
1098
0.63
628
2.44
7.98
e-02
11.4
40.
026.
140.
061.
2354
9.31
0.10
986.
098
CH
3OH
102−
9 198
6.09
816
5.40
3.13
e-03
12.4
80.
034.
400.
070.
4863
1.87
0.09
987.
560
C18
O9−
898
7.56
023
7.03
6.38
e-05
11.0
10.
143.
370.
320.
2354
0.96
0.07
987.
927
H2O
2 0,2,0−
1 1,1,0
987.
927
100.
855.
85e-
0312
.37
0.02
16.3
90.
044.
3472
66.5
90.
1899
1.32
913
CO
9−8
991.
329
237.
946.
45e-
0511
.32
0.02
6.92
0.04
1.82
6511
.49
0.11
991.
580
CH
3OH
112−
101
991.
580
190.
873.
12e-
0312
.27
0.04
5.28
0.09
0.39
591.
900.
0799
1.66
0H
2CO
140,
14−
130,
1399
1.66
036
1.28
2.97
e-02
12.2
10.
192.
460.
450.
1156
0.24
0.05
993.
108
H2S
3 0,3−
2 1,2
993.
108
102.
763.
73e-
0311
.67
0.03
5.99
0.08
0.41
643.
410.
1199
4.21
7C
H3O
H5 −
5−4 −
499
4.21
715
8.83
9.26
e-03
12.1
80.
066.
320.
140.
1762
0.99
0.08
995.
492
o-N
H3
4 0,1−
4 3,1
995.
492
285.
603.
87e-
0813
.49
0.09
0.94
0.21
0.17
801.
230.
1299
7.87
3C
H3O
H20
2−19
199
7.87
350
9.89
2.76
e-03
12.7
40.
106.
560.
230.
1368
0.72
0.07
1002
.779
H2S
3 1,3−
2 0,2
1002
.779
102.
823.
87e-
0310
.88
0.24
3.42
0.56
0.16
500.
630.
0510
05.4
55C
H3O
H21
0−20
010
05.4
5554
6.18
4.66
e-03
14.5
80.
100.
440.
220.
1064
0.46
0.07
1005
.642
CH
3OH
104−
103
1005
.642
223.
655.
06e-
0312
.41
0.07
7.31
0.16
0.12
600.
780.
0710
06.0
28C
H3O
H7 4−
7 310
06.0
2816
0.99
4.45
e-03
63B
:CH
3OH
(64−
6 3)
1006
.081
CH
3OH
6 4−
6 310
06.0
8114
4.75
4.04
e-03
63B
:CH
3OH
(74−
7 3)
1006
.111
CH
3OH
5 4−
5 310
06.1
1113
0.82
3.40
e-03
64B
:CH
3OH
(74−
7 3)
1006
.125
CH
3OH
4 4−
4 310
06.1
2511
9.21
2.26
e-03
60B
:CH
3OH
(74−
7 3)
1006
.540
CH
3OH
180−
17−
110
06.5
4040
8.23
5.12
e-03
13.4
90.
065.
140.
130.
2567
1.09
0.08
1008
.139
CH
3OH
10−
4−9 −
310
08.1
3921
5.55
4.69
e-03
12.1
60.
079.
130.
150.
2684
1.75
0.09
1008
.812
CH
3OH
5 −3−
4 −2
1008
.812
97.5
35.
63e-
0311
.93
0.04
4.85
0.09
0.47
792.
020.
1210
09.3
58C
H3O
H12−
2−11−
110
09.3
5820
7.08
2.91
e-03
12.2
20.
054.
800.
120.
2984
1.32
0.10
1011
.325
CH
3OH
171−
160
1011
.325
376.
172.
60e-
0313
.22
0.07
4.04
0.17
0.15
660.
610.
0810
13.5
63C
H3O
H10
3−9 2
1013
.563
175.
394.
29e-
0357
B:C
H3O
H(1
0 3−
9 2)
1013
.563
CH
3OH
103−
9 210
13.5
6317
5.39
4.29
e-03
57B
:CH
3OH
(10 3−
9 2)
1020
.720
CH
3OH
211−
201
1020
.720
554.
424.
88e-
0312
.61
0.05
4.32
0.12
0.16
621.
000.
0810
22.2
71C
H3O
H16
1−15
010
22.2
7132
7.24
3.49
e-03
12.5
30.
045.
290.
080.
3086
1.76
0.10
1022
.338
CH
3OH
163−
152
1022
.338
365.
373.
67e-
0312
.88
0.06
5.12
0.14
0.16
106
0.64
0.13
1023
.193
CH
3OH
8 4−
7 310
23.1
9316
3.90
8.84
e-03
63B
:CH
3OH
(84−
7 3)
1023
.197
CH
3OH
8 4−
7 310
23.1
9716
3.90
8.84
e-03
64B
:CH
3OH
(84−
7 3)
A57, page 33 of 36
A&A 556, A57 (2013)Ta
ble
A.1
.con
tinue
d.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
1024
.443
N2H
+11−
1010
24.4
4329
5.06
7.43
e-02
11.9
70.
043.
300.
090.
4194
1.78
0.11
1027
.314
CS
21−
2010
27.3
1454
2.72
2.37
e-02
11.0
40.
457.
501.
080.
1581
0.98
0.12
1028
.180
CH
3OH
163−
152
1028
.180
365.
403.
73e-
0313
.00
0.07
8.45
0.17
0.20
791.
420.
1110
32.9
98O
H+
1 1,1/2−
0 1,1/2
1032
.998
49.5
81.
41e-
0270
B:O
H+
(11,
3/2−
0 1,1/2
)10
33.0
04O
H+
1 1,3/2−
0 1,1/2
1033
.004
49.5
83.
53e-
0370
B:O
H+
(11,
1/2−
0 1,1/2
)10
33.1
12O
H+
1 1,1/2−
0 1,3/2
1033
.112
49.5
87.
03e-
0374
B:O
H+
(11,
3/2−
0 1,3/2
)10
33.1
19O
H+
1 1,3/2−
0 1,3/2
1033
.119
49.5
81.
76e-
0275
B:O
H+
(11,
1/2−
0 1,3/2
)10
35.2
47C
H3O
H12
2−11
110
35.2
4721
8.69
3.48
e-03
12.0
70.
065.
070.
150.
2899
1.41
0.12
1036
.912
CO
9−8
1036
.912
248.
887.
33e-
0511
.27
0.02
12.4
40.
0422
.64
188
257.
050.
4810
39.0
15C
H3O
H11
2−10
110
39.0
1519
0.94
3.59
e-03
12.3
10.
075.
070.
160.
4024
91.
570.
3110
42.5
22C
H3O
H6 −
5−5 −
410
42.5
2217
2.76
9.19
e-03
11.2
40.
062.
300.
140.
3010
80.
410.
1310
47.4
27C
CH
1225/2,1
3−11
23/2,1
210
47.4
2732
6.85
3.81
e-03
105
B:C
CH
(12 2
5/2,
12−
1123/2,1
1)10
47.4
27C
CH
1225/2,1
2−11
23/2,1
110
47.4
2732
6.85
3.79
e-03
98B
:CC
H(1
2 25/
2,13−
1123/2,1
2)10
47.4
90C
CH
1223/2,1
2−11
21/2,1
110
47.4
9032
6.88
3.79
e-03
93B
:CC
H(1
2 25/
2,13−
1123/2,1
2)10
47.4
90C
CH
1223/2,1
1−11
21/2,1
010
47.4
9032
6.88
3.78
e-03
92B
:CC
H(1
2 25/
2,13−
1123/2,1
2)10
56.3
55C
H3O
H11−
4−10−
310
56.3
5524
1.07
5.17
e-03
12.5
70.
045.
510.
110.
2872
1.35
0.09
1057
.118
CH
3OH
6 −3−
5 −2
1057
.118
111.
465.
86e-
0311
.90
0.03
5.93
0.07
0.44
752.
570.
1010
59.8
59C
H3O
H13−
2−12−
110
59.8
5923
7.30
3.16
e-03
12.0
90.
062.
650.
140.
2873
1.41
0.10
1061
.609
CH
3OH
113−
102
1061
.609
200.
924.
72e-
0313
.11
0.23
6.04
0.54
0.27
921.
490.
1510
62.9
81H
CN
12−
1110
62.9
8133
1.69
5.98
e-02
12.3
90.
0414
.47
0.09
0.63
124
9.19
0.22
1064
.237
CH
3OH
171−
160
1064
.237
366.
293.
98e-
0312
.44
0.05
4.49
0.12
0.28
971.
010.
1310
69.6
94H
CO
+12−
1110
69.6
9433
3.78
1.04
e-01
11.5
40.
025.
940.
060.
9256
5.86
0.07
1069
.874
CH
3OH
173−
162
1069
.874
404.
804.
14e-
0312
.86
0.06
4.01
0.15
0.14
630.
530.
0610
71.5
05C
H3O
H9 4−
8 310
71.5
0518
4.79
9.51
e-03
65B
:CH
3OH
(94−
8 3)
1071
.514
CH
3OH
9 4−
8 310
71.5
1418
4.79
9.52
e-03
66B
:CH
3OH
(94−
8 3)
1072
.837
H2S
2 2,1−
1 1,0
1072
.837
79.3
74.
13e-
0312
.33
0.14
7.48
0.33
0.31
672.
290.
0910
76.8
34C
H3O
H5 5−
4 410
76.8
3417
0.89
1.07
e-02
12.3
70.
063.
690.
130.
2887
1.01
0.12
1077
.437
CH
3OH
173−
162
1077
.437
404.
836.
26e-
0312
.68
0.28
4.80
0.67
0.16
810.
720.
1010
78.4
77C
H3O
H13
2−12
110
78.4
7724
8.84
3.88
e-03
12.3
10.
045.
310.
100.
2880
1.27
0.10
1090
.816
CH
3OH
7 −5−
6 −4
1090
.816
189.
009.
37e-
0312
.40
0.08
6.75
0.18
0.16
841.
180.
0910
92.4
63C
H3O
H12
2−11
110
92.4
6321
8.80
4.09
e-03
11.8
60.
044.
630.
100.
3590
1.66
0.10
1095
.063
CH
3OH
200−
19−
110
95.0
6349
7.93
7.23
e-03
12.4
00.
084.
120.
180.
1583
0.56
0.08
1097
.365
H2O
3 1,2,0−
3 0,3,0
1097
.365
249.
441.
64e-
0212
.66
0.02
15.6
30.
042.
1787
32.8
90.
1911
01.3
5013
CO
10−
911
01.3
5029
0.79
8.86
e-05
11.3
40.
027.
950.
041.
2675
9.39
0.13
1104
.547
CH
3OH
12−
4−11−
311
04.5
4726
8.91
5.69
e-03
12.4
20.
064.
690.
130.
2092
0.95
0.10
1105
.370
CH
3OH
7 −3−
6 −2
1105
.370
127.
716.
21e-
0312
.43
0.04
5.05
0.09
0.43
801.
940.
1011
05.9
44C
H3O
H18
1−17
011
05.9
4440
7.62
4.51
e-03
13.0
60.
053.
330.
120.
3185
1.14
0.10
1109
.585
CH
3OH
123−
112
1109
.585
228.
785.
18e-
0312
.74
0.23
5.21
0.55
0.28
971.
160.
1111
10.9
41C
H3O
H14−
2−13−
111
10.9
4126
9.85
3.40
e-03
12.7
30.
064.
870.
140.
2293
0.96
0.10
1113
.343
H2O
1 1,1,0−
0 0,0,0
1113
.343
53.4
31.
84e-
0212
.63
0.04
20.5
40.
083.
1594
48.5
80.
2211
15.2
04H
2O+
1 1,1,3/2,5/2−
0 0,0,1/2,3/2
1115
.204
53.5
23.
10e-
028.
400.
002.
500.
00−
0.22
110
−0.
890.
10
A57, page 34 of 36
M. Kama et al.: HIFI spectral survey of OMC-2 FIR 4 (CHESS)
Tabl
eA
.1.c
ontin
ued.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
1116
.986
CH
3OH
231−
221
1116
.986
659.
326.
41e-
0313
.80
0.59
5.58
1.39
0.14
119
0.65
0.11
1117
.477
N2H
+12−
1111
17.4
7734
8.69
9.68
e-02
11.7
80.
063.
480.
130.
3511
51.
230.
1211
19.8
13C
H3O
H10
4−9 3
1119
.813
207.
991.
03e-
0212
2B
:CH
3OH
(10 4−
9 3)
1119
.831
CH
3OH
104−
9 311
19.8
3120
7.99
1.03
e-02
123
B:C
H3O
H(1
0 4−
9 3)
1121
.269
CH
3OH
142−
131
1121
.269
281.
294.
30e-
0312
.23
0.07
4.55
0.17
0.15
910.
650.
1011
25.1
43C
H3O
H6 5−
5 411
25.1
4318
4.82
1.55
e-02
12.3
20.
0910
.90
0.21
0.17
991.
000.
1211
46.4
64C
H3O
H13
2−12
111
46.4
6424
8.98
4.66
e-03
12.5
60.
064.
310.
150.
3815
31.
740.
1711
47.4
15C
H3O
H19
1−18
011
47.4
1545
1.23
5.10
e-03
14.1
10.
074.
210.
170.
2916
51.
000.
1911
51.4
49H
CN
13−
1211
51.4
4938
6.95
7.63
e-02
12.1
90.
0613
.51
0.13
0.45
152
5.43
0.24
1151
.985
CO
10−
911
51.9
8530
4.17
1.01
e-04
11.4
00.
0111
.47
0.02
23.5
716
226
7.41
0.40
1153
.127
H2O
3 1,2,0−
2 2,1,0
1153
.127
249.
442.
67e-
0312
.08
0.02
16.1
30.
042.
7317
246
.14
0.39
1153
.549
CH
3OH
8 −3−
7 −2
1153
.549
146.
286.
64e-
0312
.72
0.06
5.36
0.15
0.46
140
2.07
0.17
1157
.499
CH
3OH
133−
122
1157
.499
258.
965.
66e-
0312
.52
0.46
7.96
1.14
0.35
144
1.68
0.16
1158
.727
HC
O+
13−
1211
58.7
2738
9.39
1.33
e-01
12.1
60.
187.
630.
430.
6415
45.
120.
2011
62.7
06C
H3O
H15−
2−14−
111
62.7
0630
4.74
3.61
e-03
11.5
80.
397.
870.
920.
2816
00.
990.
1111
62.9
12H
2O3 2
,1,0−
3 1,2,0
1162
.912
305.
252.
28e-
0212
.91
0.03
14.4
50.
071.
3113
718
.18
0.28
1163
.624
CH
3OH
152−
141
1163
.624
316.
054.
75e-
0313
.47
0.07
3.23
0.16
0.28
136
0.80
0.14
1168
.118
CH
3OH
114−
103
1168
.118
233.
527.
51e-
0316
1B
:CH
3OH
(11 4−
103)
1168
.150
CH
3OH
114−
103
1168
.150
233.
527.
51e-
0315
2B
:CH
3OH
(11 4−
103)
1168
.452
p-N
H3
2 1,0−
1 1,1
1168
.452
57.2
11.
21e-
0213
.06
0.26
8.38
0.60
0.54
148
3.35
0.20
1173
.435
CH
3OH
7 5−
6 411
73.4
3520
1.06
1.57
e-02
10.3
00.
087.
770.
190.
3816
51.
450.
1811
88.6
72C
H3O
H20
1−19
011
88.6
7249
7.13
5.75
e-03
12.6
90.
094.
050.
210.
2015
10.
840.
1511
99.5
99C
H3O
H4 4−
3 311
99.5
9911
9.21
1.48
e-02
12.5
80.
197.
280.
450.
3316
02.
130.
1612
00.8
55C
H3O
H14−
4−13−
312
00.8
5533
1.54
6.89
e-03
12.0
20.
084.
540.
180.
3016
00.
940.
1512
01.6
30C
H3O
H9 −
3−8 −
212
01.6
3016
7.16
7.15
e-03
11.8
90.
064.
040.
130.
5816
71.
710.
1912
05.3
68C
H3O
H14
3−13
212
05.3
6829
1.46
6.15
e-03
13.2
40.
073.
640.
160.
2615
30.
960.
1412
11.3
3013
CO
11−
1012
11.3
3034
8.93
1.18
e-04
11.9
70.
049.
030.
091.
0517
68.
770.
2812
14.8
53o-
NH
32 0
,1−
1 0,0
1214
.853
85.7
81.
81e-
0213
.79
0.04
7.57
0.08
0.91
183
5.54
0.27
1215
.246
p-N
H3
2 1,1−
1 1,0
1215
.246
58.3
21.
36e-
0219
5B
:CH
3OH
(16 −
2−15−
1)12
15.2
61C
H3O
H16−
2−15−
112
15.2
6134
1.96
5.60
e-03
204
B:p
-NH
3(2
1,1−
1 1,0
)12
16.4
20C
H3O
H12
4−11
312
16.4
2026
1.36
8.14
e-03
12.1
10.
075.
620.
180.
3419
01.
400.
1712
28.7
89H
2O2 2
,0,0−
2 1,1,0
1228
.789
195.
911.
88e-
0212
.93
0.04
12.8
00.
090.
7714
810
.18
0.28
1229
.740
CH
3OH
211−
200
1229
.740
545.
316.
45e-
0311
.30
0.14
2.25
0.34
0.34
160
0.90
0.14
1232
.476
HF
1−0
1232
.476
59.1
52.
42e-
029.
980.
082.
820.
19−
0.81
195
−2.
000.
1912
39.8
90H
CN
14−
1312
39.8
9044
6.45
9.55
e-02
12.1
90.
5614
.59
1.36
0.50
191
5.02
0.29
1249
.559
H37
Cl
2 3/2−
1 1/2
1249
.559
89.9
74.
65e-
0383
B:H
37C
l(2 3
/2−
1 5/2
)12
49.5
69H
37C
l2 3
/2−
1 5/2
1249
.569
89.9
65.
58e-
0483
B:H
37C
l(2 3
/2−
1 1/2
)12
49.5
71H
37C
l2 1
/2−
1 1/2
1249
.571
89.9
79.
30e-
0385
B:H
37C
l(2 3
/2−
1 1/2
)12
49.5
73H
37C
l2 7
/2−
1 5/2
1249
.573
89.9
71.
12e-
0283
B:H
37C
l(2 3
/2−
1 1/2
)12
49.5
73H
37C
l2 5
/2−
1 3/2
1249
.573
89.9
67.
82e-
0383
B:H
37C
l(2 3
/2−
1 1/2
)12
49.5
82H
37C
l2 3
/2−
1 3/2
1249
.582
89.9
75.
95e-
0382
B:H
37C
l(2 3
/2−
1 1/2
)12
49.5
84C
H3O
H10−
3−9 −
212
49.5
8419
0.37
1.14
e-02
84B
:H37
Cl(
2 3/2−
1 1/2
)12
49.5
95H
37C
l2 1
/2−
1 3/2
1249
.595
89.9
71.
86e-
0384
B:H
37C
l(2 3
/2−
1 1/2
)12
51.4
34H
Cl
2 5/2−
1 5/2
1251
.434
90.1
03.
36e-
0396
B:H
Cl(
2 3/2−
1 1/2
)
A57, page 35 of 36
A&A 556, A57 (2013)
Tabl
eA
.1.c
ontin
ued.
Gau
ssia
nfit
from
mom
ents
νSp
ecie
sTr
ansi
tion
ν res
tE
uA
ulv l
srδv
lsr
FW
HM
δFW
HM
T mb
rms
Flux
δFlu
xB
lend
(B)/
Not
esG
Hz
GH
zK
rad/
skm
s−1
kms−
1km
s−1
kms−
1K
mK
Kkm
s−1
Kkm
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
1251
.434
HC
l2 3
/2−
1 1/2
1251
.434
90.1
04.
67e-
0397
B:H
Cl(
2 5/2−
1 5/2
)12
51.4
47H
Cl
2 3/2−
1 5/2
1251
.447
90.1
05.
61e-
0496
B:H
Cl(
2 5/2−
1 5/2
)12
51.4
50H
Cl
2 1/2−
1 1/2
1251
.450
90.1
09.
34e-
0396
B:H
Cl(
2 5/2−
1 5/2
)12
51.4
52H
Cl
2 5/2−
1 3/2
1251
.452
90.1
07.
85e-
0396
B:H
Cl(
2 5/2−
1 5/2
)12
51.4
64H
Cl
2 3/2−
1 3/2
1251
.464
90.1
05.
98e-
0397
B:H
Cl(
2 5/2−
1 5/2
)12
51.4
81H
Cl
2 1/2−
1 3/2
1251
.481
90.1
01.
87e-
0394
B:H
Cl(
2 5/2−
1 5/2
)12
67.0
14C
O11−
1012
67.0
1436
4.97
1.34
e-04
11.6
60.
0411
.29
0.11
21.6
212
624
7.42
0.25
1496
.923
CO
13−
1214
96.9
2350
3.14
2.20
e-04
12.1
90.
0112
.02
0.02
15.9
220
919
2.13
0.44
1541
.843
CH
3OH
202−
191
1541
.843
525.
231.
06e-
0214
.84
0.05
2.56
0.11
0.58
241
1.14
0.19
1611
.794
CO
14−
1316
11.7
9458
0.50
2.74
e-04
12.3
20.
0112
.54
0.02
13.4
927
316
5.51
0.53
1661
.008
H2O
2 2,1,0−
2 1,2,0
1661
.008
194.
103.
06e-
0214
.52
0.03
10.9
90.
072.
1821
022
.30
0.33
1669
.905
H2O
2 1,2,0−
1 0,1,0
1669
.905
114.
385.
60e-
0215
.24
0.03
14.5
80.
075.
3220
066
.52
0.36
1716
.770
H2O
3 0,3,0−
2 1,2,0
1716
.770
196.
775.
06e-
0215
.01
0.02
9.91
0.05
4.70
175
53.8
60.
2817
26.6
03C
O15−
1417
26.6
0366
3.36
3.35
e-04
13.0
50.
0112
.34
0.02
10.3
422
113
5.76
0.40
1760
.486
13C
O16−
1517
60.4
8671
8.70
3.57
e-04
16.1
50.
223.
950.
510.
2617
21.
150.
1717
63.6
01p-
NH
33 1
,0−
2 1,1
1763
.601
142.
965.
28e-
0213
.83
0.15
2.13
0.36
0.40
166
3.22
0.20
1763
.823
p-N
H3
3 2,0−
2 2,1
1763
.823
126.
973.
30e-
0213
.83
0.19
2.95
0.44
0.29
169
2.05
0.18
1834
.736
OH
2 Π2 1
,−1,
0,1−
1 1,1,0,1
1834
.736
269.
762.
12e-
0289
B:O
H(2 Π
2 1,−
1,0,
2−1 1
,1,0,1
)18
34.7
47O
H2 Π
2 1,−
1,0,
2−1 1
,1,0,1
1834
.747
269.
766.
36e-
0289
B:O
H(2 Π
2 1,−
1,0,
1−1 1
,1,0,1
)18
34.7
50O
H2 Π
2 1,−
1,0,
1−1 1
,1,0,0
1834
.750
269.
764.
24e-
0289
B:O
H(2 Π
2 1,−
1,0,
1−1 1
,1,0,1
)18
37.7
47O
H2 Π
2 1,1,0,1−
1 1,−
1,0,
118
37.7
4727
0.14
2.13
e-02
85B
:OH
(2 Π2 1
,1,0,2−
1 1,−
1,0,
1)18
37.8
17O
H2 Π
2 1,1,0,2−
1 1,−
1,0,
118
37.8
1727
0.14
6.40
e-02
88B
:OH
(2 Π2 1
,1,0,1−
1 1,−
1,0,
1)18
37.8
37O
H2 Π
2 1,1,0,1−
1 1,−
1,0,
018
37.8
3727
0.14
4.27
e-02
93B
:OH
(2 Π2 1
,1,0,1−
1 1,−
1,0,
1)18
41.3
46C
O16−
1518
41.3
4675
1.73
4.05
e-04
12.6
00.
0112
.45
0.03
5.91
8369
.82
0.14
1900
.537
C+
3/2−
1/2
1900
.537
91.2
12.
32e-
069.
070.
012.
080.
0111
.58
9424
.14
0.06
A57, page 36 of 36