Desperately looking for Ly….

DRGs at z~2

Galaxies selected from near-IR photometry [(J-K)>2.3]

Most would NOT be selected by LBG criteria (UV selection)

However, overlap with LBG not quantifiedAnd certainly significant (see Adelberger Et al. 2004).

They appear in general more evolved, I.e.more massive (larger clustering), with larger stellar mass, more metal rich, and more dust obscured) than LBGs. Occurrence of AGN also seems higher.

At z~3 these galaxies have about50% of the volume density of LBGs (highly uncertaint). However; they possibly contribute about up to 100% of the LBG stellar mass density, becausethey have higher M/L ratios Van Dokkum et al. 2004

Ly to look for high-z LSS: Protoclusters

Wang et al. 2005

Identified an obvious and strong large-scale structure at redshift z~5.75 in a wide (31'×33') field, narrow-band survey of the Chandra Deep Field-South region.

This structure is traced by 17 candidate Ly emitters, among which 12 are found in an 823 nm filter (corresponding to Ly at z=5.77+/-0.03) and five in an 815 nm image (z=5.70+/-0.03).

The Ly emitters in both redshift bins are concentrated in one quadrant of the field.

Our results are consistent with reports of an overdensity in the Ultra Deep Field region at z~5.9. This structure is the highest redshift overdensity found so far.

Ly Surveys to search for LSS: Proto Superclusters

Shimasaku et al.

Ly Surveys to search for LSS

Matsuda et al.

Very useful to observestructures at the sameredshift.

LBGs not efficient to do this

The Ly Blobs

Matsuda et al.

Photo-ionization by SF orAGN?

Why so rare?

What are they?

The Ly Blobs

Matsuda et al.

H Surveys

The amplification of optical path through the ISM by resonant scatter The amplification of optical path through the ISM by resonant scatter makes Lymakes Lya fragile line: even small amount of dust can quench the a fragile line: even small amount of dust can quench the feature.feature.

Moreover, the highly unpredictable obscuration makes LyMoreover, the highly unpredictable obscuration makes Ly a poor star a poor star formation indicator.formation indicator.

HHexempt from this problem, and less subject to dust obscuration. exempt from this problem, and less subject to dust obscuration. Especially when no detections were reported in LyEspecially when no detections were reported in Lysurveys, surveys, HHwas targeted for searches to identify galaxies at high redshiftswas targeted for searches to identify galaxies at high redshifts

Problem: at z>0.4, HProblem: at z>0.4, His redshifted to the near-IR: loss of sensitivity is redshifted to the near-IR: loss of sensitivity (sky, thermal bckgnd) and of area coverage (small detector size)(sky, thermal bckgnd) and of area coverage (small detector size)

Today, identification of high-z galaxies not a problem any longer. Today, identification of high-z galaxies not a problem any longer. However, HHowever, Hsurveys still desirable to get a handle of dust surveys still desirable to get a handle of dust obscuration of SFRobscuration of SFR

H Surveys. I

Early narrow-band imaging surveys for distant galaxies Early narrow-band imaging surveys for distant galaxies were carried at the Calar Alto 3.6-m telescope:were carried at the Calar Alto 3.6-m telescope: Thompson, Mannucci & Beckwith 1996 and Beckwith Thompson, Mannucci & Beckwith 1996 and Beckwith

et al. 1998, around known QSO and radio galaxies: one et al. 1998, around known QSO and radio galaxies: one emission line galaxy at z=2.430 over 276 arcminemission line galaxy at z=2.430 over 276 arcmin22, down , down to 3.4to 3.4••1010-16-16 erg cm erg cm-2-2 s s-1-1 and most sensitive part 1.4 and most sensitive part 1.4••1010-16-16 erg cmerg cm-2-2 s s-1-1 (3 (3))

Mannucci et al. 1998, around known DLA, MgII and Mannucci et al. 1998, around known DLA, MgII and CIV QSO absorption systems: 16 HCIV QSO absorption systems: 16 H galaxies at z=2.3 galaxies at z=2.3 and 2 [OII] galaxies at z=0.89, over 163 arcminand 2 [OII] galaxies at z=0.89, over 163 arcmin22, down , down to 2to 2••1010-16-16 erg cm erg cm-2-2 s s-1-1 (3 (3))

[OIII] and H Surveys. II

Deep survey carried out from Keck with the NIRC Deep survey carried out from Keck with the NIRC instrument:instrument: Teplitz, Malkan, & McLean (1999), also around known Teplitz, Malkan, & McLean (1999), also around known

QSOs and QSO MgII and CIV QSO absorption QSOs and QSO MgII and CIV QSO absorption systems: 1 [OIII] galaxy at z=3.31 or Hsystems: 1 [OIII] galaxy at z=3.31 or H galaxy at galaxy at z=2.3 over 11 arcminz=2.3 over 11 arcmin-2-2, possibly other 12 objects, down , possibly other 12 objects, down to 7to 7••1010-17-17 erg cm erg cm-2-2 s s-1-1 (3 (3))

H Surveys. III

Near-IR observations from space with HST and NICMOS Near-IR observations from space with HST and NICMOS reach very high sensitivity thanks to fainter sky (even with reach very high sensitivity thanks to fainter sky (even with smaller telescope):smaller telescope): McCarthy et al. (1999), parallel slitless grism McCarthy et al. (1999), parallel slitless grism

spectroscopy in random fields, over 64 arcminspectroscopy in random fields, over 64 arcmin-2-2 down to down to 44••1010-17-17 erg cm erg cm-2-2 s s-1-1 (3 (3) [60% deeper than deepest ) [60% deeper than deepest ground-based survey]. Found 33 emission-line galaxies, ground-based survey]. Found 33 emission-line galaxies, likely Hlikely H at 0.7<z<1.9, with <W at 0.7<z<1.9, with <Wee>=40 Ang.>=40 Ang.

Median Ha luminosity is 2.7Median Ha luminosity is 2.7••10104242 erg s erg s, and star-, and star-formation rates in the range 1<SFR<324 Mformation rates in the range 1<SFR<324 MOO yr yr, with , with <SFR>=21M<SFR>=21MOO yr yr

H Surveys From Space

McCarthy et al. (1999)

H Surveys From Space

McCarthy et al. (1999)

H Surveys From Space: Sensitivity

McCarthy et al. (1999)

McCarthy et al. (1999)

McCarthy et al. (1999)

McCarthy et al. (1999)

H Surveys Results: SFR Diagnostic Tresse et al. 2002, MNRAS, 337, 369, Ha LF up to z~1Tresse et al. 2002, MNRAS, 337, 369, Ha LF up to z~1 Hopkins, A & Connolly, A. 2000, ApJ, 129, 2843, SFR in galaxies Hopkins, A & Connolly, A. 2000, ApJ, 129, 2843, SFR in galaxies

at .7<z<1.8 from NICMOS grism parallel Ha survey. Find average 2-at .7<z<1.8 from NICMOS grism parallel Ha survey. Find average 2-3 higher SFR from Ha than from UV, as seen locally.3 higher SFR from Ha than from UV, as seen locally.

Teplitz et al. 2003, ApJ, 589, 704, STIS Parallel Survey, survey for Teplitz et al. 2003, ApJ, 589, 704, STIS Parallel Survey, survey for [OII]; implies substantial extinction[OII]; implies substantial extinction

Drozdovsky et al. 2005, ApJ, 130, 1324, ACS grism parallel survey Drozdovsky et al. 2005, ApJ, 130, 1324, ACS grism parallel survey for ELGs at z<1.6, [OII], Hfor ELGs at z<1.6, [OII], H, [OIII], H, [OIII], H

Doherty et al. 2006, MNRAS, 370, 331, HDoherty et al. 2006, MNRAS, 370, 331, H w/ CIRPAS of HDF-N w/ CIRPAS of HDF-N FFFF

Kicks, et al. 2002, ApJ, 581, 205, NICMOS parallel Ha survey. Kicks, et al. 2002, ApJ, 581, 205, NICMOS parallel Ha survey. Derive downward revised calibration of [OII]; also revised Derive downward revised calibration of [OII]; also revised diagnostics diagnostics

All conclude SF increase ~(1+z)All conclude SF increase ~(1+z)3-43-4 to z~1, find extinction affects UV to z~1, find extinction affects UV by ~3x, find [II] traces SF.by ~3x, find [II] traces SF.

H Surveys Results: SF Diagnostics Mouhcine et al. 2005, MNRAS, 362, 1143, ratio of [OII]/HMouhcine et al. 2005, MNRAS, 362, 1143, ratio of [OII]/H of 2dF of 2dF

galaxies, difference from Madrid due to selection effects (Hgalaxies, difference from Madrid due to selection effects (H selection vs. B-band selection)selection vs. B-band selection)

Moustakas, Kennicutt, Tremonti 2006, ApJ, 642, 775, dust-obscured Moustakas, Kennicutt, Tremonti 2006, ApJ, 642, 775, dust-obscured HH good indicator of SFR, even in highly obscured SF galaxies. good indicator of SFR, even in highly obscured SF galaxies. [OII] can be calibrated as a SFR indicator, and dependence of [OII] can be calibrated as a SFR indicator, and dependence of metallicity reduced.metallicity reduced.

Mustakas, Kennicutt, 2006, ApJ, 651, 155, Unlike the integrated RMustakas, Kennicutt, 2006, ApJ, 651, 155, Unlike the integrated R2323 parameter, we find that the integrated [N II]/Hparameter, we find that the integrated [N II]/Hand [S II]/Hand [S II]/H ratios ratios are enhanced with respect to line ratios typical of H II regions, are enhanced with respect to line ratios typical of H II regions, consistent with a modest contribution from diffuse ionized gas consistent with a modest contribution from diffuse ionized gas emission. We conclude that the Remission. We conclude that the R2323 parameter can be used to reliably parameter can be used to reliably measure the gas-phase abundances of distant star-forming galaxies. measure the gas-phase abundances of distant star-forming galaxies.

H Surveys Results: SF DiagnosticsHicks et al. 2002

Optical spectra of 14 emission-line galaxies from the NICMOS H survey of McCarthy et al. are presented.

Of the 14, 9 have emission lines confirming the redshifts found in the grism survey. The higher resolution of the new spectra improves the redshift accuracy by a factor of 5.

The [O II]/H values are found more than 2 times lower than expected from Jansen et al.

This [O II]/H ratio discrepancy most likely explained by additional reddening in our H-selected sample [on average, as much as an extra E(B-V)=0.6], as well as by a possible stronger dependence of the [O II]/H ratio on galaxy luminosity than is found in local galaxies.

The result is that star formation rates (SFRs) calculated from [O II]3727 emission, uncorrected for extinction, are found to be on average 4+/-2 times lower than the SFRs calculated from H emission.

Classification of emission-line galaxies as starburst or Seyfert galaxies based on comparison of the ratios [O II]/H and [Ne III]3869/H is discussed.

New Seyfert 1 diagnostics using the H line luminosity, H-band absolute magnitude, and H equivalent widths are also presented. One galaxy is classified as a Seyfert 1 based on its broad emission lines, implying a comoving number density for Seyfert 1 galaxies of 2.5+5.9

-2.1×10-5 Mpc-3, a factor of 2.4+5.5-2.0 times higher than

estimated by other surveys.

H Surveys Results: SF Diagnostics at z~2

Erb et al. 2006:

UV and H can be used as tracers of SF in distant SF galaxies that are not too obscured by dust.

The history of the cosmic star formation activity (madau diagram)In the local universe, Ha survey are key to measure theSFD:

Zamorano et al. 1994, 1996; Alonso et al. 1995Gallego, J et al. 1995

At High-z contunuum-based measures preferred. But Lya might help at the faint end of LF

At z~6 the cosmic star formation activity was ~as vigorous as it was between z~2 and z~3.

Giavalisco et al. 2004Giavalisco et al. 2006, in prep.

=-1.6 assumed

Mergers? Disks? Star-formation in filaments of cold gas in DM halos? Ravindranath et al. 2006

35 kpc (180 comoving)

H Rotation curves at z~2

GOODS large area and angular resolutionenabled the first systematic kinematical studies of galaxies at z~2

Erb et al. 2004Steidel et al. 200413 GOODS-N galaxies

morphologically selected

H Rotation curves at z~2

What is the relationship between morphology and kinematics?

HDF-BX691

Only 3 out of 13 galaxies showevidence of coherent velocityfield/shear

Erb et al. 2004

Steidel et al. 2004

Galaxy kinematics at z~2

Erb et al. 2004

Elongated galaxies appear to have lower velocity dispersions

Still small samples. More Hspectroscopic time needed

Ha IFU spectroscopy at z~2: Evidence for Disks

Galaxies with irregular morphologies appear to be disks

Already dynamically assembled at z~2

Implicataions could be that mering rate estimated from Distorted morphology is (possibly greatly) overestimated

Forster-Schreiber et al. 2006

Ha IFU spectroscopy at z~2: Evidence for Disks

Forster-Schreiber et al. 2006

[OIII] Surveys: Planetary Nebulae

Mendez et al. 2001