J/MNRAS/415/1479 LESS photometric redshift survey (Wardlow+, 2011)
The LABOCA survey of the Extended Chandra Deep Field-South: a photometric redshift survey of submillimetre galaxies. Wardlow J.L., Smail I., Coppin K.E.K., Alexander D.M., Brandt W.N., Danielson A.L.R., Luo B., Swinbank A.M., Walter F., Weiss A., Xue Y.Q., Zibetti S., Bertoldi F., Biggs A.D., Chapman S.C., Dannerbauer H., Dunlop J.S., Gawiser E., Ivison R.J., Knudsen K.K., Kovacs A., Lacey C.G., Menten K.M., Padilla N., Rix H.-W., Van Der Werf P.P. <Mon. Not. R. Astron. Soc., 415, 1479-1508 (2011)> =2011MNRAS.415.1479W
ADC_Keywords: Millimetric/submm sources ; Galaxies, IR ; Galaxies, photometry Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: starburst - submillimetre: galaxies Abstract: We derive photometric redshifts from 17-band optical to mid-infrared photometry of 78 robust radio, 24um and Spitzer IRAC counterparts to 72 of the 126 submillimetre galaxies (SMGs) selected at 870um by LABOCA observations in the Extended Chandra Deep Field-South (ECDF-S). We test the photometric redshifts of the SMGs against the extensive archival spectroscopy in the ECDF-S. Description: SMGs typically have faint optical and near-IR counterparts (e.g. Ivison et al. 2002MNRAS.337....1I), so we require deep photometry for accurate photometric redshift estimates. The ECDF-S was chosen for this survey because it is an exceptionally well-studied field and as such we are able to utilize data from extensive archival imaging and spectroscopic surveys. For completeness and uniformity, we only consider surveys that cover a large fraction of the ECDF-S rather than the smaller and deeper central Chandra Deep Field-South (CDF-S) region. Therefore, we utilize the MUltiwavelength Survey by Yale-Chile (MUSYC; Gawiser et al. 2006, Cat. J/ApJS/162/1) near-IR survey for U- to K-band imaging (Taylor et al. 2009, Cat. J/ApJS/183/295), and the Spitzer IRAC/MUSYC Public Legacy in ECDF-S (SIMPLE) imaging for Spitzer IRAC data (Damen et al. 2011, cat. J/ApJ/727/1). We also include U-band data from the deep GOODS/VIMOS imaging survey of the CDF-S (Nonino et al. 2009ApJS..183..244N); although this covers only ∼60 per cent of LESS SMGs, it is valuable for galaxies that are undetected at short wavelengths in the shallower MUSYC survey. In addition, we have carried out deep near-IR observations in the J and Ks bands with the HAWK-I at the ESO-VLT (ID: 082.A-0890, PI: N. Padilla). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 210 78 Observed photometry for robust counterparts to LESS submillimetre galaxies (SMGs) table3.dat 132 78 *The catalogue of 78 robust counterparts to LESS submillimetre galaxies (SMGs)
Note on table3.dat: their photometric redshift estimates, reduced χ2 of the best-fitting SED and the number of photometric filters in which the galaxy is observed. We also present the absolute rest-frame H-band magnitudes, the derived FIR luminosities and characteristic dust temperatures of the SMGs.
See also: J/ApJ/707/1201 : LABOCA ECDFS Submillimeter Survey (LESS) (Weiss+, 2009) J/MNRAS/413/2314 : submm galaxies radio and mid-IR counterpart (Biggs+, 2011) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [LESS] 6- 8 I3 --- LESS LESS sequential number (short name) (1) 9 A1 --- m_LESS [ab] Multiplicity index on Name 11 A1 --- l_UmagM Limit flag on UmagM (2) 12- 16 F5.2 mag UmagM ?=- MUSYC U magnitude 18- 21 F4.2 mag e_UmagM ? rms uncertainty on MUSYC U magnitude 23 A1 --- l_U38mag Limit flag on U38mag (2) 24- 28 F5.2 mag U38mag ?=- MUSYC U38 magnitude 30- 33 F4.2 mag e_U38mag ? rms uncertainty on MUSYC U38 magnitude 35 A1 --- l_UmagV Limit flag on UmagV (2) 36- 40 F5.2 mag UmagV ?=- VIMOS U magnitude 42- 45 F4.2 mag e_UmagV ? rms uncertainty on VIMOS U magnitude 47 A1 --- l_BmagV Limit flag on BmagV (2) 48- 52 F5.2 mag BmagV ?=- VIMOS B magnitude 54- 57 F4.2 mag e_BmagV ? rms uncertainty on VIMOS B magnitude 59 A1 --- l_VmagV Limit flag on VmagV (2) 60- 64 F5.2 mag VmagV ?=- VIMOS V magnitude 66- 69 F4.2 mag e_VmagV ? rms uncertainty on VIMOS V magnitude 71 A1 --- l_RmagV Limit flag on RmagV (2) 72- 76 F5.2 mag RmagV ?=- VIMOS R magnitude 78- 81 F4.2 mag e_RmagV ? rms uncertainty on VIMOS R magnitude 83 A1 --- l_ImagV Limit flag on ImagV (2) 84- 88 F5.2 mag ImagV ?=- VIMOS I magnitude 90- 93 F4.2 mag e_ImagV ? rms uncertainty on VIMOS I magnitude 95 A1 --- l_zmagV Limit flag on zmagV (2) 96-100 F5.2 mag zmagV ?=- VIMOS z magnitude 102-105 F4.2 mag e_zmagV ? rms uncertainty on VIMOS z magnitude 107 A1 --- l_JmagM Limit flag on JmagM (2) 108-112 F5.2 mag JmagM ?=- MUSYC J magnitude 114-117 F4.2 mag e_JmagM ? rms uncertainty on MUSYC J magnitude 119 A1 --- l_JmagH Limit flag on JmagH (2) 120-124 F5.2 mag JmagH ?=- HAWK-I J magnitude 126-129 F4.2 mag e_JmagH ? rms uncertainty on HAWK-I J magnitude 131 A1 --- l_HmagH Limit flag on HmagH (2) 132-136 F5.2 mag HmagH ?=- HAWK-I H magnitude 138-141 F4.2 mag e_HmagH ? rms uncertainty on HAWK-I H magnitude 143 A1 --- l_KmagM Limit flag on KmagM (2) 144-148 F5.2 mag KmagM ?=- MUSYC K magnitude 150-153 F4.2 mag e_KmagM ? rms uncertainty on MUSYC K magnitude 155 A1 --- l_KmagH Limit flag on KmagH (2) 156-160 F5.2 mag KmagH ?=- HAWK-I K magnitude 162-165 F4.2 mag e_KmagH ? rms uncertainty on HAWK-I K magnitude 167-171 F5.2 mag [3.6] ?=- Spitzer/IRAC 3.6um magnitude 173-176 F4.2 mag e_[3.6] ? rms uncertainty on IRAC 3.6um magnitude 178-182 F5.2 mag [4.5] ?=- Spitzer/IRAC 4.5um magnitude 184-187 F4.2 mag e_[4.5] ? rms uncertainty on IRAC 4.5um magnitude 189-193 F5.2 mag [5.8] Spitzer/IRAC 5.8um magnitude 195-198 F4.2 mag e_[5.8] rms uncertainty on IRAC 5.8um magnitude 200 A1 --- l_[8.0] Limit flag on 8.0um (2) 201-205 F5.2 mag [8.0] ?=- Spitzer/IRAC 8.0um magnitude 207-210 F4.2 mag e_[8.0] ? rms uncertainty on IRAC 8.0um magnitude
Note (1): SMGs which are not covered by imaging in a given filter have no photometry listed in that filter. Note (2): 3σ limiting magnitudes are presented where sources are covered by imaging but not detected.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [LESS] 6- 21 A16 --- SMG LESS name (JHHMMSS.s+DDMMSS) (3) 23- 26 A4 --- --- [LESS] 28- 30 I3 --- LESS LESS sequential number (short name) 31 A1 --- m_LESS [ab] Multiplicity index on Name 33- 34 I2 h RAh Right ascension (J2000) (4) 36- 37 I2 min RAm Right ascension (J2000) (4) 39- 43 F5.2 s RAs Right ascension (J2000) (4) 45 A1 --- DE- Declination sign (J2000) (4) 46- 47 I2 deg DEd Declination (J2000) (4) 49- 50 I2 arcmin DEm Declination (J2000) (4) 52- 55 F4.1 arcsec DEs Declination (J2000) (4) 57- 60 F4.2 --- zph Photometric redshift (5) 62- 65 F4.2 --- E_zph Error on zph (upper value) 67- 70 F4.2 --- e_zph Error on zph (lower value) 72- 75 F4.1 --- chi2r Reduced chi^2^ value (6) 77- 78 I2 --- Nf Number of photometric filters in which each SMG counterpart was detected 80- 81 I2 --- Nf2 Number of filters in which the SMG was observed but not detected, providing a limiting flux 84- 89 F6.2 mag HMAG Absolute magnitude in the rest-frame H band 91 A1 --- l_LFIR Limit flag on LFIR 92- 97 F6.2 TLsun LFIR FIR luminosity, in 10^12^L☉ (7) 99-104 F6.2 TLsun E_LFIR ? Error on LFIR (upper value) 106-111 F6.2 TLsun e_LFIR ? Error on LFIR (lower value) 112 A1 --- l_TD Limit flag on TD 113-117 F5.1 K TD Characteristic dust temperature (8) 119-122 F4.1 K E_TD ? Error on TD (upper value) 124-127 F4.1 K e_TD ? Error on TD (lower value) 129-130 A2 --- Type [RMI ] ID type (9) 132 A1 --- Note [*] Note on LESS 20 (10)
Note (3): The SMG names correspond to those in Weiss et al. (2009, Cat. J/ApJ/707/1201) and Biggs et al. (2011, Cat. J/MNRAS/413/2314). Note (4): Coordinates are the J2000 position of the optical/near-IR counterpart. Note (5): Since Hyperz was restricted to 0<z<7, the five galaxies whose upper redshift limits yield a formal maximum redshift of zmax=7 are actually only constrained in the lower redshift limit. Therefore, throughout this paper, the redshifts of these galaxies are plotted as lower limits. Note (6): Reduced χ2 of the best-fitting SED at the derived photometric redshift. Note (7): As discussed in Section 5.7, the FIR luminosity (LFIR) is derived from the IR-radio correlation using the radio flux and the photometric redshift of each SMG. Note (8): The characteristic dust temperature (TD) is derived as discussed in Section 5.7 from radio and submillimetre fluxes and the photometric redshift of each SMG. Note (9): ID types (see Biggs et al. 2011 Cat. J/MNRAS/413/2314for details) as follows: R = radio-identified counterpart M = 24um-identified counterpart I = IRAC-identified counterpart Note (10): As shown in Section 5.1, LESS 20 appears to contain a radio-loud AGN. Therefore, LFIR and TD presented here are likely significantly overestimated due to the AGN contribution to the radio flux, as such LESS 20 is excluded from our studies of the luminosity function, SFR and star formation history of SMGs (Section 5.7).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Feb-2012
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