J/ApJ/788/125 An ALMA survey of ECDFS submillimeter galaxies (Simpson+, 2014)
An ALMA survey of submillimeter galaxies in the extended Chandra Deep
Field-South: the redshift distribution and evolution of submillimeter galaxies.
Simpson J.M., Swinbank A.M., Smail I., Alexander D.M., Brandt W.N.,
Bertoldi F., de Breuck C., Chapman S.C., Coppin K.E.K., da Cunha E.,
Danielson A.L.R., Dannerbauer H., Greve T.R., Hodge J.A., Ivison R.J.,
Karim A., Knudsen K.K., Poggianti B.M., Schinnerer E., Thomson A.P.,
Walter F., Wardlow J.L., Weiss A., van der Werf P.P.
<Astrophys. J., 788, 125 (2014)>
=2014ApJ...788..125S 2014ApJ...788..125S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, millimetric/submm ;
Photometry, UBVRIJKLMNH ; Redshifts
Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: starburst
Abstract:
We present the first photometric redshift distribution for a large
sample of 870 µm submillimeter galaxies (SMGs) with robust
identifications based on observations with ALMA. In our analysis we
consider 96 SMGs in the Extended Chandra Deep Field South, 77 of which
have 4-19 band photometry. We model the SEDs for these 77 SMGs,
deriving a median photometric redshift of zphot=2.3±0.1. The remaining
19 SMGs have insufficient photometry to derive photometric redshifts,
but a stacking analysis of Herschel observations confirms they are not
spurious. Assuming that these SMGs have an absolute H-band magnitude
distribution comparable to that of a complete sample of z∼1-2 SMGs,
we demonstrate that they lie at slightly higher redshifts, raising the
median redshift for SMGs to zphot=2.5±0.2. Critically we show that
the proportion of galaxies undergoing an SMG-like phase at z≥3 is at
most 35%±5% of the total population. We derive a median stellar mass
of M*=(8±1)x1010 M☉, although there are systematic
uncertainties of up to 5x for individual sources. Assuming that the
star formation activity in SMGs has a timescale of ∼100 Myr, we show
that their descendants at z∼0 would have a space density and MH
distribution that are in good agreement with those of local ellipticals.
In addition, the inferred mass-weighted ages of the local ellipticals
broadly agree with the look-back times of the SMG events. Taken
together, these results are consistent with a simple model that
identifies SMGs as events that form most of the stars seen in the
majority of luminous elliptical galaxies at the present day.
Description:
In this study we undertake a multi-wavelength analysis of the
ALMA-detected submm galaxies from the catalog presented by Hodge et al.
(2013, J/ApJ/768/91) (see also Karim et al. 2013MNRAS.432....2K 2013MNRAS.432....2K). To
briefly summarize the observations, we obtained 120 s integrations
of 122 of the original 126 LESS submm sources, initially identified
using the LABOCA camera on the APEX telescope (Weiss et al. 2009,
J/ApJ/707/1201). These Cycle 0 observations used the compact
configuration, yielding a median synthesized beam of ∼1.6"x1.2". The
observing frequency was matched to the original LESS survey, 344 GHz
(Band 7), and we reach a typical rms across our velocity-integrated
maps of 0.4 mJy/beam.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 98 19 Summary of Photometry
table2.dat 214 96 Photometry
table3.dat 84 77 Derived Properties
--------------------------------------------------------------------------------
See also:
J/ApJS/155/73 : Photometric redshifts of X-ray sources in CDF-S
(Zheng+, 2004)
J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)
J/ApJ/699/1610 : Spitzer survey of submillimeter galaxies (Hainline+, 2009)
J/ApJ/707/1201 : LABOCA ECDFS Submillimeter Survey (LESS) (Weiss+, 2009)
J/ApJS/191/124 : Optical spectroscopy of ECDF-S X-ray sources
(Silverman+, 2010)
J/ApJS/203/15 : Counterparts to 1.4GHz sources in ECDF-S (Bonzini+, 2012)
J/ApJ/768/91 : ALMA observations of LESS submm galaxies (Hodge+, 2013)
J/MNRAS/442/577 : Selected ALESS submm galaxies radio properties
(Thomson+, 2014)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Filter Filter used in the observation
21- 24 F4.2 um lambda Effective wavelength
26- 29 F4.1 --- Limit 3σ detection limit in AB mag
31- 48 A18 --- r_Limit Detection limit reference
50- 68 A19 --- Bibcode Reference bibcode
70- 83 A14 --- Cat Catalog reference in VizieR
85- 98 A14 --- Com Comment on reference
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- --- [ALESS]
7- 11 A5 --- ALESS SMG identifier (NN.NN; NNN.N) (1)
13 A1 --- f_ALESS [a] Flag on ALESS (2)
15 A1 --- l_UMmag [>] The 3σ upper limit on UMmag
17- 21 F5.2 mag UMmag ? MUSYC U band magnitude
23- 26 F4.2 mag e_UMmag ? Uncertainty in UMmag
28 A1 --- l_U38mag [>] The 3σ upper limit on U38mag
30- 34 F5.2 mag U38mag ? MUSYC U38 band magnitude
36- 39 F4.2 mag e_U38mag ? Uncertainty in U38mag
41 A1 --- l_UVmag [>] The 3σ upper limit on UVmag
43- 47 F5.2 mag UVmag ? VIMOS U band magnitude
49- 52 F4.2 mag e_UVmag ? Uncertainty in UVmag
54 A1 --- l_Bmag [>] The 3σ upper limit on Bmag
56- 60 F5.2 mag Bmag ? MUSYC WFI B band magnitude
62- 65 F4.2 mag e_Bmag ? Uncertainty in Bmag
67 A1 --- l_Vmag [>] The 3σ upper limit on Vmag
69- 73 F5.2 mag Vmag ? MUSYC WFI V band magnitude
75- 78 F4.2 mag e_Vmag ? Uncertainty in Vmag
80 A1 --- l_Rmag [>] The 3σ upper limit on Rmag
82- 86 F5.2 mag Rmag ? MUSYC WFI R band magnitude
88- 91 F4.2 mag e_Rmag ? Uncertainty in Rmag
93 A1 --- l_Imag [>] The 3σ upper limit on Imag
95- 99 F5.2 mag Imag ? MUSYC WFI I band magnitude
101-104 F4.2 mag e_Imag ? Uncertainty in Imag
106 A1 --- l_zmag [>] The 3σ upper limit on zmag
108-112 F5.2 mag zmag ? MUSYC Mosaic-II z band magnitude
114-117 F4.2 mag e_zmag ? Uncertainty in zmag
119 A1 --- l_Jmag [>] The 3σ upper limit on Jmag
121-125 F5.2 mag Jmag ? J band magnitude (TENIS if nothing in f_Ksmag)
(3)
127-130 F4.2 mag e_Jmag ? Uncertainty in Jmag
132-133 A2 --- f_Jmag Flag on Jmag (4)
135 A1 --- l_Hmag [>] The 3σ upper limit on Hmag
137-141 F5.2 mag Hmag ? H band magnitude
143-146 F4.2 mag e_Hmag ? Uncertainty in Hmag
148 A1 --- l_Ksmag [>] The 3σ upper limit on Ksmag
150-154 F5.2 mag Ksmag ? KS band magnitude (TENIS if nothing
in f_Ksmag) (3)
156-159 F4.2 mag e_Ksmag ? Uncertainty in Ksmag
161-162 A2 --- f_Ksmag [* **] Flag on Ksmag and Jmag (4)
164 A1 --- l_3.6mag [>] The 3σ upper limit on 3.6mag
166-170 F5.2 mag 3.6mag SIMPLE/IRAC 3.6 micron band magnitude
172-175 F4.2 mag e_3.6mag ? Uncertainty in 3.6mag
177 A1 --- l_4.5mag [>] The 3σ upper limit on 4.5mag
179-183 F5.2 mag 4.5mag SIMPLE/IRAC 4.5 micron band magnitude
185-188 F4.2 mag e_4.5mag ? Uncertainty in 4.5mag
190 A1 --- l_5.8mag [>] The 3σ upper limit on 5.8mag
192-196 F5.2 mag 5.8mag ? SIMPLE/IRAC 5.8 micron band magnitude
198-201 F4.2 mag e_5.8mag ? Uncertainty in 5.8mag
203 A1 --- l_8.0mag [>] The 3σ upper limit on 8.0mag
205-209 F5.2 mag 8.0mag ? SIMPLE/IRAC 8.0 micron band magnitude
211-214 F4.2 mag e_8.0mag ? Uncertainty in 8.0mag
--------------------------------------------------------------------------------
Note (1): All photometry is left blank where a source is not covered by
available imaging.
Note (2): Flag as follows:
a = Source is within 4" of a 3.6 micron source of comparable, or greater,
flux.
Note (3): We measure J and KS photometry from three imaging surveys, but quote
a single value, in order of 3σ detection limit (see Table 1).
Note (4): Flag as follows:
* = Photometry measured from HAWK-I imaging;
** = Photometry measured from MUSYC imaging,
otherwise photometry measured from TENIS imaging.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- --- [ALESS]
7- 12 A6 --- ALESS SMG identifier (NNN.NN)
14 A1 --- f_ALESS [a] Flag on ALESS (1)
16- 17 I2 h RAh Hour of Right Ascension (J2000)
19- 20 I2 min RAm Minute of Right Ascension (J2000)
22- 26 F5.2 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 38 F4.1 arcsec DEs Arcsecond of Declination (J2000)
40- 43 F4.2 --- zphot Photometric redshift
45- 48 F4.2 --- E_zphot Upper limit uncertainty in zphot
50- 53 F4.2 --- e_zphot Lower limit uncertainty in zphot
55- 58 F4.2 --- zspec ? Spectroscopic redshift
60 A1 --- r_zspec zspec reference (2)
62- 66 F5.2 --- Chi2 Reduced Χ2
68- 69 I2 --- Detec Number of detection
71- 72 I2 --- Obs Number of observation
74- 79 F6.2 mag HMag Absolute H band AB magnitude
81- 84 F4.2 Msun/Lsun M/L H band mass-to-light ratio
--------------------------------------------------------------------------------
Note (1): Flag as follows:
a = As discussed in Section 3.2.1 these SMGs are potential gravitational
lenses, or have significantly contaminated photometry. We advise that the
photometric redshifts for these SMGs are treated with extreme caution.
Note (2): Reference as follows:
b = Casey et al. (2011MNRAS.411.2739C 2011MNRAS.411.2739C);
c = Zheng et al. (2004, J/ApJS/155/73);
d = Swinbank et al. (2012MNRAS.427.1066S 2012MNRAS.427.1066S);
e = Silverman et al. (2010, J/ApJS/191/124);
f = Kriek et al. (2008ApJ...677..219K 2008ApJ...677..219K);
g = Coppin et al. (2009MNRAS.395.1905C 2009MNRAS.395.1905C);
h = Coppin et al. (2012MNRAS.427..520C 2012MNRAS.427..520C); Danielson et al. in prep;
i = Bonzini et al. (2012, J/ApJS/203/15).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 17-Jul-2017