direct-detection spectroscopy at the cso with z-spec and zeus
DESCRIPTION
Direct-Detection Spectroscopy at the CSO with Z-Spec and ZEUS. Probing galaxies near and far with two new bolometers-based grating spectrometers Matt Bradford with input from Gordon Stacey August 4, 2008. Dominant gas coolants are in the far-IR / submm Redshifted to the submm / mm. - PowerPoint PPT PresentationTRANSCRIPT
Matt Bradford 1
Direct-Detection Spectroscopy at the CSO with
Z-Spec and ZEUS
Probing galaxies near and far withtwo new bolometers-based grating
spectrometers
Matt Bradford with input from Gordon StaceyAugust 4, 2008
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 2CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Dominant gas coolants are in the far-IR / submmRedshifted to the submm / mm
SED courtesy A. Blain CO
C0
N+
C+
O0
O++
CSO @ z=0CSO @ z=1.2
CSO @ z=2.6
CSO @ z=4.4
Matt Bradford 3
Direct-Detection SpectroscopyA survey capability which complements the high spatial and spectral
resolution of interferometers (CARMA / ALMA) Submillimeter is the region of overlap between coherent (heterodyne) and
incoherent (direct-detection) techniques for astrophysics. Coherent approaches have yielded much of the spectroscopic work to date.
High spectral resolution required for Galactic cores. Large bandwidths not essential for Galactic sources or nearby galaxies. SIS mixers near quantum limit, (also near background limit at 1 mm). Until recently, direct detectors neither sufficiently sensitive, nor sufficiently arrayed to
be compelling. Direct-detection spectrometers (gratings and Fabry-Perots) for long wavelengths are
large and expensive. Direct-detection submillimeter spectrometers are now compelling
Submillimeter spectroscopy coming of age as an extragalactic probe. Spectral resolution greater than few x 1000 not required. Direct detectors are now readily background-limited, and are undergoing a revolution
in format (driven by cameras). Large fractional bandwidth presents a new discovery space for measuring
redshifts and multiple lines. Multi-object capability a natural progression with a direct-detection system.
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
The World’s Only Submillimeter Grating Spectrometers
ZEUSThe Redshift (z) and Early Universe Spectrometer
Stacey et al. (Cornell) w/ GSFC, NIST Short submm windows: 350mm, 450 mm Slit-fed echelle grating, 4th and 5th order Resolving power ~1200 (300 km/s) 20 GHz (~2-4%) instantaneous bandwidth 1x32 bolometer array, but TES upgrade underway
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 4
Z-SpecGlenn (U. Colorado); Bradford, Bock, Zmuidzinas,
(Caltech), Aguirre (CU-> Penn), Matsuhara (ISAS) 1 mm window: 195-310 GHz Single beam w/ new waveguide grating architecture Resolving power ~300 (1000 km/s) 100 GHz (40%) instantaneous bandwidth 160 individually-mounted Ge-sensed bolometers
Both with sensitivity very close to fundamental limits at the CSO
Matt Bradford 5
Primary Scientific Objectives Embedded energy sources and conditions of star forming gas in
local-universe infrared-bright galaxies (LIRGS and ULIRGS).
Interstellar medium conditions and spatial extent of star formation extent in the era of peak star-formation history (z=0.5 to 2) and prior.
Evolutionary history of energy release via unbiased redshift surveys.
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
ZEUSJ=6->5 and 7->6 in both 12CO and 13CO
and [CI] J=2->1 constrain the mass and energy budget of the warm molecular gas.
Z-Spec Complete 1-mm spectrum includes multiple
high-critical-density species: CN, CS, HCN, HNC, HCO+. A rapid census of the dense molecular gas.
ZEUSC+ at z=1--1.2 and 1.8--2. C+ to dust
continuum ratio measures the UV field intensity, constrains the extent of the starburst.
Access [OI], [NII], [OIII] at the highest redshifts.
Z-SpecFull band provides at least 2 CO transitions
to measure redshift as well as temperature, density, and mass of the molecular gas.
Unexplored rest-frame short-submm.C+, other fine-structure transitions
accessible beyond z=6.
Matt Bradford 6
35 cm long R2 echelle grating blazed for 5th order @ 359 mm There is a series of a scatter, quartz, 2 long pass, and a bandpass filter in series to achieve
dark performance (Cardiff U.) Total optical efficiency: ~ 30%, or 15% including bolometer DQE
Dual Stage 3He
Refrigerator
4He cryostat
M5: Primary
Grating
Detector Array
Scatter Filter
LP Filter 1
LP Filter 2
BP Filter Wheel
M1
M2
M3
M4
M6
4He Cold
Finger
Entrance Beamf/12
Grating
Quartz & LP Filter 1
Refrigerator
ZEUS: Optical Path
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 7
ZEUS on the CSO Mounted on the left Nasmyth focus Has been co-mounted and co-scheduled
with both Z-Spec and Bolocam First light in 2006 Thesis project of Steve Hailey-Dunsheath
(Cornell PhD 2008)
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 8
ZEUS observations of NGC 253: First Extragalactic Detection of 13CO(6-5)
Line is bright ~ 10% that of the 12CO(6-5) line indicating optically thick emission in the main line.
We also re-observed (and mapped) the CO(7-6) line to constrain LVG models
35 to 55% of the molecular ISM is warm and dense: T~ 120 K, n~104 cm-3
Heating this much gas is difficult:likely due to that X-rays from the starburst or the decay of micro-turbulence within clouds must dominate the heating.
These processes are powered by the starburst -> the starburst is self-regulating.
Hailey-Dunsheath et al. in prep.
12CO(6-5)13CO(6-5)10
T MB(K
)
vLSR(km/s)
T MB(K
)
vLSR(km/s)
CO(7-6)
[CI] (2-1)
12CO(6-5)13CO(6-5)10
12CO(6-5)13CO(6-5)10
T MB(K
)
vLSR(km/s)
T MB(K
)
vLSR(km/s)
CO(7-6)
[CI] (2-1)
ZEUS/CSO
[CI] (2-1) line only 1000 km/s to the blue and always within ZEUS band.
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 9
ZEUS Observations of LIRGs & ULIRGs Pre-ZEUS: 1 ULIRG in CO 6-5
(Mrk 231, Papadopoulos et al. 07) ZEUS has observed ~19 LIRGs
and ULIRGs to date Most in CO (6-5) Some also in CO (7-6) & [CI]
(2-1) or CO (8-7) Fractional mid-J CO luminosity
decreases in the most powerful sources (as with C+).
-> More concentrated systems than the less-luminous starbursts.
Nikola et al. in prep.
-0.05
0
0.05
0.1
0.15
0.2
3000 4000 5000 6000 7000 -0.010
0.000
0.010
0.020
0.030
4000 5000 6000 7000
-0.04
0.00
0.04
0.08
0.12
0.16
5200 6200 7200 8200
Arp 220 CO(6-5)
NGC 6240 CO(6-5)
IRAS 18293CO(6-5)
T MB(
K)
-0.025
0
0.025
0.05
0.075
11000 12000 13000 14000
-0.05
0.00
0.05
0.10
0.15
0.20
0.25
5700 6700 7700
VLSR(km/s) VLSR(km/s)
IRAS 17208 CO(6-5)
NGC 6240 [CI] (2-1) & CO (7-6)
-0.05
0.00
0.05
0.10
0.15
0.20
0.25
5500 7500
vLSR [km/s]
T MB [K
]
NGC 6240 CO(8-7)
Arp 220
NGC 6240
Zw049M 82
Arp 299
IRAS17208
Mrk 231
L>1012
L>1011
L<1011
0.0
1.0
2.0
3.0
4.0
9 10 11 12 13
log(LFIR/LSUN)
CO(6
-5)/F
(60
μm)
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 10
ZEUS High-Redshift Example: [CII] from MIPS J142824.0 +352619
Identified as red object in MIPS Bootes field (Borys et al. 2006)
Integrated far-IR SED indicates Lfar-IR ~ 3.21013 L
Likely a mildly lensed super-starburst galaxy
ZEUS/CSO detection in April 2008 -- 1.5 hours of good (but not great) weather (225 GHz ~ 0.05 to 0.06) I[CII] ~ 6 K-km/sec Fline ~ 9.0 10-18 W m-2
L[CII] ~ 2.5 1010 L CII / far-IR ratio much greater
than in local ULIRGs. Conclude that starburst is 2-3 kpc in extent – “galaxy wide starburst”
Hailey-Dunsheath et al. 2008
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
-1000 -500 0 500 1000 1500
T MB
(mK
)
VLSR w.r.t. z = 1.3249
MIPS J142824.0+352619
[CII] at z = 1.3249
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
-1000 -500 0 500 1000 1500
T MB
(mK
)
VLSR w.r.t. z = 1.3249
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
-1000 -500 0 500 1000 1500
T MB
(mK
)
VLSR w.r.t. z = 1.3249
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
-1000 -500 0 500 1000 1500
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
MIPS J142824.0+352619 [CII] @ z=1.3249
-10
-5
0
5
10
15
20
1828.51044.5260.5-523.5
ZEUS/CSO
-1000 -500 0 500 1000 1500-1000 -500 0 500 1000 1500
T MB
(mK
)
VLSR w.r.t. z = 1.3249
MIPS J142824.0+352619
[CII] at z = 1.3249
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 11
Z-Spec: A New Ultracompact Waveguide Grating
Propagation confined in parallel-plate waveguide 2-D Geometry Stray light eliminated
Curved grating diffracts and focuses Efficient use of space No additional optical elements
Custom “stigmatic” grating design possible at long wavelengths H.A. Rowland, 1883, Phil. Mag 16
K.A. McGreer, 1996, IEEE Phot. Tech. 8
curved grating in parallel plate waveguide
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 12CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Z-Spec Layout
FRIDGE
Focal ARC
GRATING ARC
ADR
INPUTFEEDHORN
3He RADIATION SHIELD
Individually mountedSiN bolometers
CSO, Mauna Kea
Matt Bradford 13CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Z-Spec graduate students @ 13,400 ft Lieko Earle (Colorado), Bret Naylor (Caltech)
Z-Spec 1 mm survey of NGC 253Lieko Earle, U. Colorado Ph.D. ‘08
3.5 hours telescope time19 ID’d transitions > 3s+4 unID’d as of yet.
Z-Spec Spectra from the CSO
Z-Spec Spectra from the CSO
Matt Bradford 17CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Molecular Gas in Local-Universe Galaxies, ex. M82 B. Naylor et al., ApJ in prep.
HCO+
Compile all transitions, use RADEX to model excitation & transfer in the lines-> Generate Bayesian likelihoods
NE
SW
Cen
Also include:CSHNCSO2
Combine in a single model:-> evidence of cold, dense gas component -> the material actually forming the stars?
Matt Bradford 18CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 19CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 20CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
APM 08279+5255 at z=3.91
Matt Bradford 21
Water Stacking of APM ?
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 22
Plans for the next cycleZEUS & Z-Spec instrument programs funded
ZEUS upgrade to ZEUS-2Funded by NSF MRI
Incorporating (3) NIST 2-d TES bolometer arrays which share the focal plane and can operate simultaneously: 10 x 24 at 200 mm 9 x 40 at 350-450 mm 5 x 12 at 650 mm
Up to 5 lines simultaneously (in extended sources)
Some imaging capability (9-10 beams)
Closed cycle refrigerators
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Z-Spec Survey ProgramFunded by NSF AAG
(Aguirre et al. U. Penn)
Dense gas in Local-Universe dense molecular gas surveys. 50 galaxies, 8 hours per
Mid-J CO + spectral discovery in high-z objects with and without prior redshifts. 20 galaxies, 24 hours per
Excellent use of low-frequency time at CSO. Baseline 300 hours per year,
could be more. Helium recycler under study
to reduce cryogen costs.
Matt Bradford 23
Backup material
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 24
[CII]/far-IR Constrains Starburst Extent
L[CIII] ~ 2.5 1010 L
Lfar-IR ~ 3.2 1013 L
30% of [CII] from ionized mediumR = 5.5 10-4 G ~ 2000
far-IR = L/(4D2) = 14 DL~ 9.2 Gpc
= IR/(G 2) = 3.5 x 10-3 = beam = 0.083(”)2
d ~ 0.32” 2.75 kpc
Starlight that contributes to but not G
[CII]/far-IR continuum luminosity ratio vs. density for various G (from Kaufman 1999).
+3600- 700
Galaxy-wide starburst supports the contention that hyper-luminous systems may be giant elliptical
galaxies in formation (unlike local ULIRGs)
CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Matt Bradford 25CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
Range: 185--305 GHz• Resolving
power: 250--400
(Not over sampled)(750 < v < 1200 km/s)• Complete
coverage from channel to channel -> no gaps
Z-Spec channel spectral responseMeasured with long-path FTS(~100 MHz resolution)
Relative to an imaging system, fundamental noise levels are lower, but some systematic aspects are easier.
Chopping -> response to a single frequency
Narrow spectrometer bandwidth helpsNEFsky ~ NEFGaussian noise ~ sqrt()
Scaling consistent with e.g. Bolocam observations
Z-Spec SensitivityObserved noise white with atmospheric 1/f
500
300
Blue -> achieved at =0, 0.1, 0.2Black -> simple model for Z-Spec at CSO Det, amplifier, & internal load NEP: 6.4e-18 W/sqrt(Hz) (not tracking detector parameters in detail) measured instrument trans (~0.25) Aperture efficiency per taper + Ruze (60-70%) measured chop duty cycle (65%) photon noise from sky + telescope the most important term -> additional factor of 1.2
Z-Spec SensitivityClear scaling with , very close to photon background limit
=0
=0.1
=0.2
Bret NaylorRecent Caltech Ph.D.
James Aguirre -> U. PennJansky FellowColorado, NRAO
Lieko EarleColorado Ph.D. student(finishing Spring 08)
Z-Spec labor force
Matt Bradford 29CSO NSF Reverse Site Visit: Arlington, VA 2008 Aug 4
ULIRG Survey Preliminary Results
Galaxy cz Log L CO CN HCN HNC HCO+ HCN/CO HNC/HCN HCO+/HCN
M82 250 10.8 16803 749 202 169 799 0.009 0.84 3.95
NGC 1068 1137 11.5 6590 432 317 91 219 0.036 0.29 0.69
Arp 220 5434 12.0 1418 76 275 243 81 0.144 0.88 0.29NGC6240 7340 11.8 1596 53 68 <20 88 0.031 <0.29 1.31Mrk273 11326 12.1 342 47 41 20 19 0.089 0.48 0.47NGC4418 11782 11.7 367 47 106 42 30 0.215 0.40 0.28UGC5101 11809 12.0 301 22 22 19 13 0.055 0.84 0.57Mrk231 12650 12.2 536 76 54 41 44 0.075 0.76 0.81IRAS 17208 12834 12.4 570 29 47 47 25 0.061 0.99 0.53
Starburst
Seyferts
ULIRGS
Not finding overluminous HNC / HCN 3-2 ratio as per Aalto, Cernicharo.will follow-up further at CSO.
[ Line fluxes in Jy km/s, HCN / CO ratio corrected for to TMB ]Line fluxes SNR 4 - 20
Nearby Seyfert NGC 1068
Z-Spec Commissioning At CSO