J/ApJ/902/78 ALMA 3mm new sp. redshifts for SPT galaxies (Reuter+, 2020)
The complete redshift distribution of dusty star-forming galaxies from the
SPT-SZ survey.
Reuter C., Vieira J.D., Spilker J.S., Weiss A., Aravena M.,
Archipley M., Bethermin M., Chapman S.C., De Breuck C., Dong C.,
Everett W.B., Fu J., Greve T.R., Hayward C.C., Hill R., Hezaveh Y.,
Jarugula S., Litke K., Malkan M., Marrone D.P., Narayanan D., Phadke K.A.,
Stark A.A., Strandet M.L.
<Astrophys. J., 902, 78 (2020)>
=2020ApJ...902...78R 2020ApJ...902...78R
ADC_Keywords: Galaxies, spectra; Redshifts; Surveys; Millimetric/submm sources
Keywords: Observational cosmology ; Early universe ; High-redshift galaxies ;
Galaxy evolution ; Interstellar molecules
Abstract:
The South Pole Telescope (SPT) has systematically identified
81 high-redshift, strongly gravitationally lensed, dusty star-forming
galaxies (DSFGs) in a 2500 square degree cosmological millimeter-wave
survey. We present the final spectroscopic redshift survey of this
flux-limited (S870µm>25mJy) sample, initially selected at 1.4mm.
The redshift survey was conducted with the Atacama Large
Millimeter/submillimeter Array across the 3mm spectral window,
targeting carbon monoxide line emission. By combining these
measurements with ancillary data, the SPT sample is now
spectroscopically complete, with redshifts spanning 1.9<z<6.9 and a
median of z=3.9±0.2. We present the millimeter through far-infrared
photometry and spectral energy density fits for all sources, along
with their inferred intrinsic properties. Comparing the properties of
the SPT sources to the unlensed DSFG population, we demonstrate that
the SPT-selected DSFGs represent the most extreme infrared-luminous
galaxies, even after accounting for strong gravitational lensing. The
SPT sources have a median star formation rate of
2.3(2)x103M☉/yr and a median dust mass of
1.4(1)x109M☉. However, the inferred gas depletion timescales
of the SPT sources are comparable to those of unlensed DSFGs, once
redshift is taken into account. This SPT sample contains roughly half
of the known spectroscopically confirmed DSFGs at z>5, making this the
largest sample of high-redshift DSFGs to date, and enabling the
"high-redshift tail" of extremely luminous DSFGs to be measured.
Though galaxy formation models struggle to account for the SPT
redshift distribution, the larger sample statistics from this complete
and well-defined survey will help inform future theoretical efforts.
Description:
In order to obtain redshifts for the South Pole Telescope (SPT)
sample, a blind spectroscopic redshift search was started in ALMA
Cycle 0 (project ID: 2011.0.00957.S).
An updated distribution was presented in Strandet+ (2016ApJ...822...80S 2016ApJ...822...80S)
with an additional 15 sources observed in ALMA Cycle 1
(project ID: 2012.1.00844.S).
This work represents the conclusion of the SPT blind redshift survey,
and presents spectroscopic scans for the remaining 40 sources from
ALMA Cycles 3, 4, and 7, and 41 new spectroscopic redshifts.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 56 81 Positions of SPT-selected DSFGs, obtained by
fitting ALMA 3mm continuum images
tabled1.dat 89 81 Photometry for all SPT-selected sources
tablee1.dat 162 81 Redshifts and line identifications
tablef1.dat 89 81 Individual source properties
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See also:
VIII/103 : Herschel Multi-tiered Extragalactic Survey (Oliver+, 2012)
VIII/95 : Herschel Multi-tiered Extragalactic Survey (Oliver+, 2012)
J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)
J/ApJ/707/1201 : LABOCA ECDFS Submillimeter Survey (LESS) (Weiss+, 2009)
J/ApJ/719/763 : Millimeter-wave sources in the SPT survey (Vieira+, 2010)
J/ApJ/779/61 : SPT-SZ point sources at 95, 150 & 220GHz (Mocanu+, 2013)
J/MNRAS/444/117 : Luminous (sub-)millimetre galaxies (Koprowski+, 2014)
J/MNRAS/439/1556 : ACT high significance 148 & 218GHz sources (Marsden+, 2014)
J/ApJ/788/125 : An ALMA survey of ECDFS submm galaxies (Simpson+, 2014)
J/ApJ/806/110 : ALESS survey: SMGs in the ECDF-S data (da Cunha+, 2015)
J/MNRAS/462/1989 : HerMES Large Mode Survey catalogue (Asboth+, 2016)
J/ApJ/832/78 : SCUBA-2 & LABOCA obs. of HATLAS red galaxies (Ivison+, 2016)
J/A+A/608/A15 : ALMA survey of submm gal. in COSMOS field (Brisbin+, 2017)
J/ApJ/840/78 : Redshift survey of ALMA SMGs in ECDFS (Danielson+, 2017)
J/ApJ/849/L36 : mm-wave size study of ALMA submm galaxies (Ikarashi+, 2017)
J/MNRAS/469/492 : JCMT/SCUBA2 objects in COSMOS and UDS (Michalowski+ 2017)
J/ApJ/839/58 : ALMA submm galaxies multi-wavelength data (Simpson+, 2017)
J/ApJ/862/96 : Star-forming gal. with LABOCA 870um obs. (Lewis+, 2018)
J/A+A/609/A30 : Conversion factors to LIR & Mdust (Schreiber+, 2018)
J/ApJ/900/55 : The SPT-SZ catalog at 95, 150, and 220GHz (Everett+, 2020)
J/A+A/635/A7 : NOEMA redshift of bright Herschel galaxies (Neri+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- AName Abbreviated name (SPTHHMM+DD)
12- 16 A5 --- --- [SPT-S]
18- 32 A15 --- SPT-S Name of the source (<SPT-S JHHMMSS+DDMM.m>;
but 3 sources: <SPT-S JHHMMSS+DDMM.mm>) (1)
34- 35 I2 h RAh Hour of right ascension (J2000)
37- 38 I2 min RAm Minute of right ascension (J2000)
40- 44 F5.2 s RAs Second of right ascension (J2000)
46 A1 --- DE- Sign of declination (J2000)
47- 48 I2 deg DEd Degree of declination (J2000)
50- 51 I2 arcmin DEm Arcminute of declination (J2000)
53- 56 F4.1 arcsec DEs Arcsecond of declination (J2000)
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Note (1): SPT-S J230721-4930.4 is not part of the final 81 selected dusty
star-forming galaxies (DSFGs); removed from this table by CDS.
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- AName Abbreviated name (SPTHHMM+DD)
12- 16 F5.3 --- zsp [1.86/6.91] Spectroscopic redshift
18- 21 F4.2 mJy S3000um [0.16/8.82]? 3000um flux density
23- 26 F4.2 mJy e_S3000um [0.02/0.5]? S3000um uncertainty (2)
28- 31 F4.1 mJy S2000um [0.7/24] 2000um flux density (3)
33- 35 F3.1 mJy e_S2000um [0.4/2] S2000um uncertainty (2)
37- 38 I2 mJy S1400um [3/67] 1400um flux density (3)
40- 41 I2 mJy e_S1400um [2/12] S1400um uncertainty (2)
43- 45 I3 mJy S870um [26/200] 870um flux density
47- 48 I2 mJy e_S870um [3/12] S870um uncertainty (2)
50- 52 I3 mJy S500um [37/555] 500um flux density
54- 55 I2 mJy e_S500um [5/15] S500um uncertainty (2)
57- 59 I3 mJy S350um [38/758] 350um flux density
61- 62 I2 mJy e_S350um [5/20] S350um uncertainty (2)
64 A1 --- l_S250um Limit flag on S250um (4)
66- 68 I3 mJy S250um [19/796] 250um flux density
70- 71 I2 mJy e_S250um [4/37]? S250um uncertainty (2)
73 A1 --- l_S160um Limit flag on S160um (4)
75- 77 I3 mJy S160um [22/532]? 160um flux density
79- 80 I2 mJy e_S160um [8/59]? S160um uncertainty (2)
82 A1 --- l_S100um Limit flag on S100um (4)
84- 86 I3 mJy S100um [1/239]? 100um flux density
88- 89 I2 mJy e_S100um [2/11]? S100um uncertainty (2)
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Note (2): The uncertainties do not include absolute calibration errors.
Note (3): The 2mm and 1.4mm SPT flux densities are deboosted and were presented
in Everett et al. (2020, J/ApJ/900/55).
Note (4): Non-detections are shown as 3σ upper limits.
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Byte-by-byte Description of file: tablee1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- AName Abbreviated name (SPTHHMM+DD)
12- 15 A4 --- Cycle ALMA Cycle in which the 3mm scan was obtained
17- 23 F7.5 --- zsp [1.86/6.91] Spectroscopic redshift (5)
25- 31 F7.5 --- e_zsp [5e-05/0.04] Redshift uncertainty
33 A1 --- f_zsp [z] z=3mm spectrum obtained using Z-Spec
35- 43 A9 --- Fig Figure number(s) in the paper
45- 54 A10 --- rms Typical rms found in each ALMA 3mm spectrum,
given a channel width of 62.5MHz
56- 85 A30 --- lines Lines from 3mm scans
87- 89 A3 --- r_lines Reference(s) (6)
91-156 A66 --- Comm New lines and comments indicating any
follow-up spectroscopy or photometric redshift
158-162 A5 --- r_Comm Reference(s) (6)
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Note (5): The values for spectroscopic redshift differ slightly from previous
works because the data was binned to a common binning and was fitted
through MCMC. The spectroscopic redshifts obtained, however, are
consistent within their error bars to previously published data.
Note (6): References as follows:
a = Published by Strandet et al. (2016ApJ...822...80S 2016ApJ...822...80S).
b = Published by Weiss et al. (2013ApJ...767...88W 2013ApJ...767...88W).
c = Published by Aravena et al. (2016MNRAS.457.4406A 2016MNRAS.457.4406A).
d = Published by Gullberg et al. (2015MNRAS.449.2883G 2015MNRAS.449.2883G).
e = Published by Aravena et al. (2013MNRAS.433..498A 2013MNRAS.433..498A).
f = Published by Spilker et al. (2015ApJ...811..124S 2015ApJ...811..124S).
g = Published by Spilker et al. (2014ApJ...785..149S 2014ApJ...785..149S).
h = Published by Strandet et al. (2017ApJ...842L..15S 2017ApJ...842L..15S).
i = Published by Marrone et al. (2018Natur.553...51M 2018Natur.553...51M).
j = Obtained as part of ALMA project ID: 2017.1.01340.S.
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Byte-by-byte Description of file: tablef1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- AName Abbreviated name (SPTHHMM+DD)
12- 16 F5.3 --- zsp [1.86/6.91] Spectroscopic redshift
18- 20 F3.1 --- zph [1.9/6.8] Photometric redshift
22- 24 F3.1 --- e_zph [0.3/1.3] zph uncertainty
26- 27 I2 K Tdust [21/79] Dust temperature (7)
29- 30 I2 K e_Tdust [2/31] Tdust uncertainty
32- 34 I3 um lamPk [56/154] Peak wavelength
36- 37 I2 um e_lamPk [2/14] lamPk uncertainty
39- 43 F5.2 --- mu [1/32.7] Gravitational amplification (µ)
45- 49 F5.2 --- e_mu [0/17.51]? mu uncertainty
51- 53 A3 --- f_mu Flag on mu
55- 58 F4.2 10+13Lsun LFIR [0.1/3.7] FIR luminosity (7)
60- 63 F4.2 10+13Lsun e_LFIR [0.02/0.7] LFIR uncertainty
65- 69 F5.2 10+9Msun Mdust [0.11/17.23] Dust mass (8)
71- 75 F5.2 10+9Msun e_Mdust [0.02/19.52] Lower uncertainty on Mdust
77- 80 F4.2 10+9Msun E_Mdust [0.01/6.67] Upper uncertainty on Mdust
82- 85 F4.1 10+3Msun/yr SFR [0.3/18.1] Star formation rate (8)
87- 89 F3.1 10+3Msun/yr e_SFR [0.1/5] SFR uncertainty
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Note (7): Estimates of dust temperatures and FIR luminosities are derived
from the modified blackbody fits described in Section 2.3.2.
Note (8): Using dust temperatures and FIR luminosities, the dust masses and
SFRs are then derived using Equation (2) and Equation (3),
respectively; see Section 2.3.3. While not explicitly given in the
table, the total IR luminosity can be obtained using the SFR, as shown
in Equation (3). The FIR luminosities, SFRs and dust masses were
corrected for gravitational amplification (µ) according to Table D1
of Spilker+ (2016ApJ...826..112S 2016ApJ...826..112S) where such models exist. Where
multiple source components exist, we use a flux-weighted average to
estimate µ. Though the intrinsic values are presented above, the
apparent values can be obtained by multiplying by the magnification factor.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 13-Apr-2022