J/ApJ/864/8 High resolution NIR observations of z≳1 galaxies (Lacy+, 2018)
A subarcsecond near-infrared view of massive galaxies at z>1 with Gemini
Multi-conjugate Adaptive Optics.
Lacy M., Nyland K., Mao M., Jagannathan P., Pforr J., Ridgway S.E.,
Afonso J., Farrah D., Guarnieri P., Gonzales-Solares E., Jarvis M.J.,
Maraston C., Nielsen D.M., Petric A.O., Sajina A., Surace J.A., Vaccari M.
<Astrophys. J., 864, 8 (2018)>
=2018ApJ...864....8L 2018ApJ...864....8L
ADC_Keywords: Galaxies, IR; Photometry, ugriz; Redshifts
Keywords: galaxies: evolution
Abstract:
We present images taken using the Gemini South Adaptive Optics Imager
(GSAOI) with the Gemini Multi-conjugate Adaptive Optics System (GeMS)
in three 2arcmin2 fields in the Spitzer Extragalactic Representative
Volume Survey. These GeMS/GSAOI observations are among the first ∼0.1"
resolution data in the near-infrared spanning extragalactic fields
exceeding 1.5' in size. We use these data to estimate galaxy sizes,
obtaining results similar to those from studies with the Hubble Space
Telescope, though we find a higher fraction of compact star-forming
galaxies at z>2. To disentangle the star-forming galaxies from active
galactic nuclei (AGNs), we use multiwavelength data from surveys in
the optical and infrared, including far-infrared data from Herschel,
as well as new radio continuum data from the Australia Telescope
Compact Array and Very Large Array. We identify ultraluminous infrared
galaxies (ULIRGs) at z∼1-3, which consist of a combination of pure
starburst galaxies and AGN/starburst composites. The ULIRGs show signs
of recent merger activity, such as highly disturbed morphologies and
include a rare candidate triple-AGN. We find that AGNs tend to reside
in hosts with smaller scale sizes than purely star-forming galaxies of
similar infrared luminosity. Our observations demonstrate the
potential for MCAO to complement the deeper galaxy surveys to be made
with the James Webb Space Telescope.
Description:
The three asterisms observed are drawn from three different Spitzer
Extragalactic Representative Volume Survey (SERVS) fields:
ELAIS-S1 (centered on RAJ2000=00:37:48,DEJ2000=-44:00),
XMM-LSS (centered on RAJ2000=02:20:00,DEJ2000=-04:48), and
CDFS (centered on RAJ2000=03:32:19,DEJ2000=-28:06). All SERVS fields
were observed to the same depth (20 minutes) during the post-cryogenic
Spitzer mission in the 3.6 and 4.5um bands, with the observational
scheme described in Mauduit+ (2012PASP..124.1135M 2012PASP..124.1135M) reaching a 5σ
depth of ∼2uJy in each band.
The three fields were observed in Gemini program GS-2013B-Q14. ES1-C
is in the SERVS ELAIS-S1 field (observed on 2014 Dec 03), XMM-C2 is in
the XMM-LSS field (observed on 2014 Dec 10-11), and CDFS-C is in the
CDFS field (observed on 2015 Jan 04).
The ES1-C field was observed in four runs with the Australia Telescope
Compact Array (ATCA) at 8.4GHz, 2016 March 10-13. We obtained 56hr
of data. The XMM-C2 field was observed in a single pointing with the
VLA in A-configuration as part of project VLA/14A-353 over the
frequency range 8-12GHz.
The ES1 field of SERVS was observed with the Cerro Tololo
Inter-American Observatory (CTIO) Mosaic II camera in the i band in
two runs, one on 2009 November 25, and the other from 2010 September
30 to 2010 October 4.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 313 165 Optical through near-infrared Tractor photometry
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See also:
III/334 : VISTA Deep Extragalactic Observations (VIDEO) (Jarvis+, 2013)
II/359 : The VISTA Hemisphere Survey (VHS) catalog DR4.1 (McMahon+, 2013)
VIII/95 : Herschel Multi-tiered Extragalactic Survey (Oliver+, 2012)
J/ApJ/586/794 : Multiwavelength luminosities of galaxies (Bell, 2003)
J/ApJ/735/86 : NEWFIRM MBS: photometric catalogs (Whitaker+, 2011)
J/ApJS/203/24 : Structural param. of galaxies in CANDELS (van der Wel+, 2012)
J/ApJS/219/15 : Morphologies of z=0-10 galaxies with HST data (Shibuya+, 2015)
J/ApJ/827/L25 : Fractions of quiescent galaxies evolution (Martis+, 2016)
J/ApJS/230/9 : Improved multi-band photometry from SERVS (Nyland+, 2017)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- ID Source identifier in catalog
11- 20 F10.7 deg RAdeg Right Ascension (J2000)
22- 32 F11.7 deg DEdeg [-44.1/-4.5] Declination (J2000)
34- 45 F12.9 arcsec Rad [-1.8/2.3] Half-light radius (1)
47- 61 F15.8 --- ell [-44583/8.5] Ellipticity
63- 77 F15.7 deg PA [-386275/585] Position angle; East of North
79- 81 A3 --- Mod Model fit (2)
83- 93 F11.3 uJy F4.5 [0.7/232541] SERVS Spitzer/IRAC 4.5um band
flux density
95-105 F11.3 uJy F3.6 [-0.3/232541] SERVS Spitzer/IRAC 3.6um band
flux density
107-116 F10.3 uJy FKs [-0.5/8357] VIDEO VISTA Ks band flux density
118-127 F10.3 uJy FH [-0.4/7530] VIDEO VISTA H band flux density
129-138 F10.3 uJy FJ [-0.8/8503] VIDEO VISTA J band flux density
140-149 F10.3 uJy FY [-0.2/16178]? VIDEO VISTA Y band flux density
151-160 F10.3 uJy FZV [-0.3/8542] VIDEO VISTA ZV band flux density
162-171 F10.3 uJy Fz0 [0.002/2977]? z0 band flux density
173-181 F9.3 uJy Fi [-0.02/1015] i band flux density
183-192 F10.3 uJy Fr [-0.2/1626] r band flux density
194-203 F10.3 uJy Fg [-0.07/1626] g band flux density
205-214 F10.3 uJy Fu [-0.09/1969]? u band flux density
216-222 F7.3 uJy e_F4.5 [0.03/0.2] Uncertainty in F4.5 (3)
224-230 F7.3 uJy e_F3.6 [0.03/0.2] Uncertainty in F3.6 (3)
232-237 F6.3 uJy e_FKs [0.3/2.2] Uncertainty in FKs (3)
239-244 F6.3 uJy e_FH [0.2/1.2] Uncertainty in FH (3)
246-251 F6.3 uJy e_FJ [0.1/1.5] Uncertainty in FJ (3)
253-259 F7.3 uJy e_FY [0.1/0.5]? Uncertainty in FY (3)
261-267 F7.3 uJy e_FZV [0.05/0.4] Uncertainty in FZV (3)
269-275 F7.3 uJy e_Fz0 [0.02/0.1]? Uncertainty in FZ0 (3)
277-283 F7.3 uJy e_Fi [0.01/0.6] Uncertainty in Fi (3)
285-291 F7.3 uJy e_Fr [0.007/0.3] Uncertainty in Fr (3)
293-299 F7.3 uJy e_Fg [0.005/0.4] Uncertainty in Fg (3)
301-307 F7.3 uJy e_Fu [0.009/0.3]? Uncertainty in Fu (3)
309-313 F5.3 --- z [0.01/5.4] Best EAZY photometric redshift
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Note (1): A value of zero indicates a point source was fit.
Note (2): Model fit as follows:
dev = de Vaucouleurs profile;
exp = exponential disk;
pt = point source.
Note (3): The flux errors are statistical errors from the surface brightness
profile fits performed during the Tractor photometry and do not
include calibration errors.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Aug-2019