J/ApJ/769/116 Dust-obscured galaxies in the local universe (Hwang+, 2013)
Dust-obscured galaxies in the local universe.
Hwang H.S., Geller M.J.
<Astrophys. J., 769, 116 (2013)>
=2013ApJ...769..116H 2013ApJ...769..116H
ADC_Keywords: Photometry, infrared ; Photometry, ultraviolet ;
Photometry, SDSS ; Galaxies, IR ; Redshifts ; Surveys
Keywords: galaxies: active; galaxies: evolution; galaxies: formation;
galaxies: starburst; infrared: galaxies; surveys
Abstract:
We use Wide-field Infrared Survey Explorer (WISE), AKARI, and Galaxy
Evolution Explorer (GALEX) data to select local analogs of
high-redshift (z∼2) dust obscured galaxies (DOGs). We identify 47
local DOGs with S12µm/S0.22µm≥892 and S12µm>20mJy at
0.05<z<0.08 in the Sloan Digital Sky Survey data release 7. The
infrared (IR) luminosities of these DOGs are in the range
3.4x1010(L☉)≲LIR≲7.0x1011(L☉) with a median LIR
of 2.1x1011(L☉). We compare the physical properties of local
DOGs with a control sample of galaxies that have lower
S12µm/S0.22µm but have similar redshift, IR luminosity, and
stellar mass distributions. Both WISE 12µm and GALEX
near-ultraviolet (NUV) flux densities of DOGs differ from the control
sample of galaxies, but the difference is much larger in the NUV.
Among the 47 DOGs, 36%±7% have small axis ratios in the optical
(i.e., b/a<0.6), larger than the fraction among the control sample
(17%±3%). There is no obvious sign of interaction for many local
DOGs. No local DOGs have companions with comparable optical magnitudes
closer than ∼50kpc. The large- and small-scale environments of DOGs
are similar to the control sample. Many physical properties of local
DOGs are similar to those of high-z DOGs, even though the IR
luminosities of local objects are an order of magnitude lower than for
the high-z objects: the presence of two classes (active galactic
nuclei- and star formation-dominated) of DOGs, abnormal faintness in
the UV rather than extreme brightness in the mid-IR, and diverse
optical morphology. These results suggest a common underlying physical
origin of local and high-z DOGs. Both seem to represent the high-end
tail of the dust obscuration distribution resulting from various
physical mechanisms rather than a unique phase of galaxy evolution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 90 47 Properties of WISE 12um selected DOGs
table2.dat 79 47 UV and optical photometry for WISE 12um selected DOGs
table3.dat 95 47 NIR and MIR photometry for WISE 12um selected DOGs
table4.dat 91 47 MIR and FIR photometry for WISE 12um selected DOGs
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See also:
V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/298 : AKARI/FIS All-Sky Survey Point Source Catalogues (ISAS/JAXA, 2010)
II/297 : AKARI/IRC mid-IR all-sky Survey (ISAS/JAXA, 2010)
II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
J/ApJ/744/150 : Dust-obscured galaxies (DOGs) at z≃2 (Bussmann+, 2012)
J/AJ/143/125 : SED of 113 dust-obscured galaxies at z∼2 (Melbourne+, 2012)
J/A+A/533/A119 : GOODS-Herschel North and South catalogs (Elbaz+, 2011)
J/ApJS/182/628 : Spitzer quasar and ULIRG evolution study (Veilleux+, 2009)
J/ApJ/692/422 : MAMBO observations of SWIRE sources (Lonsdale+, 2009)
J/ApJ/663/81 : SED of hard X-ray selected AGN in XMDS (Polletta+, 2007)
J/ApJS/173/293 : UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)
J/PASP/117/227 : Properties of 101 galaxies from the NFGS (Kewley+, 2005)
J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/47] Running sequence number
4- 22 I19 --- objID SDSS-DR9 ObjID
24- 25 I2 h RAh Hour of right ascension (J2000)
27- 28 I2 min RAm Minute of right ascension (J2000)
30- 34 F5.2 s RAs Second of right ascension (J2000)
36 A1 --- DE- Sign of declination (J2000)
37- 38 I2 deg DEd Degree of declination (J2000)
40- 41 I2 arcmin DEm Arcminute of declination (J2000)
43- 47 F5.2 arcsec DEs Arcsecond of declination (J2000)
49- 54 F6.4 --- z [0.05/0.08] Redshift
56- 60 F5.2 10+10Msun M* [1.56/41.95]? Stellar mass (1)
62- 66 F5.2 10+10Msun e_M* [0.34/10.45]? M* uncertainty (1)
68 A1 --- l_Lir Limit flag on Lir
70- 74 F5.2 10+10Lsun Lir [3.42/68.74] IR luminosity
76- 79 F4.2 10+10Lsun e_Lir [0.09/5.9]? Lir uncertainty
81 A1 --- l_fAGN Limit flag on fAGN
83- 85 I3 % fAGN [0/100] AGN contribution to the total
IR luminosity
87- 88 I2 % e_fAGN [0/10]? fAGN uncertainty
90 A1 --- Cl Classification (2)
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Note (1): Stellar masses for the galaxies without SDSS spectra are not
available.
Note (2): Galaxy classification based on optical line ratios as follows:
H = star formation activity,
C = Composite,
S = Seyfert,
L = LINER,
U = Undetermined.
The lower case letter gives the classification adopted from NED.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/47] Running sequence number
4- 8 F5.2 mag FUV [19.5/22.7]? GALEX FUV magnitude (3)
10- 13 F4.2 mag e_FUV [0.05/0.5]? FUV uncertainty (3)
15- 19 F5.2 mag NUV [18.3/22.8] GALEX NUV magnitude (3)
21- 24 F4.2 mag e_NUV [0.04/0.7] NUV uncertainty (3)
26- 30 F5.2 mag umag [16.6/20.5] SDSS Petrosian u-band magnitude (3)
32- 35 F4.2 mag e_umag [0.02/0.7] umag uncertainty (3)
37- 41 F5.2 mag gmag [15.3/18.4] SDSS Petrosian g-band magnitude (3)
43- 46 F4.2 mag e_gmag [0/0.4] gmag uncertainty (3)
48- 52 F5.2 mag rmag [14.6/17.6] SDSS Petrosian r-band magnitude (3)
54- 57 F4.2 mag e_rmag [0/0.4] rmag uncertainty (3)
59- 63 F5.2 mag imag [14.3/17.2] SDSS Petrosian i-band magnitude (3)
65- 68 F4.2 mag e_imag [0/0.4] imag uncertainty (3)
70- 74 F5.2 mag zmag [14.1/17] SDSS Petrosian z-band magnitude (3)
76- 79 F4.2 mag e_zmag [0.01/0.3] zmag uncertainty (3)
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Note (3): All magnitudes are Galactic extinction-corrected AB magnitudes.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/47] Running sequence number
4- 8 F5.2 mag Jmag [13.7/16.3]? 2MASS J-band magnitude (4)
10- 13 F4.2 mag e_Jmag [0.03/0.2]? Jmag uncertainty
15- 19 F5.2 mag Hmag [13.3/16]? 2MASS H-band magnitude (4)
21- 24 F4.2 mag e_Hmag [0.03/0.2]? Hmag uncertainty
26- 30 F5.2 mag Ksmag [13/16]? 2MASS Ks-band magnitude (4)
32- 35 F4.2 mag e_Ksmag [0.03/0.2]? Ksmag uncertainty
37- 41 F5.2 mJy S3.4 [0.7/36.5] WISE 3.4um flux density
43- 46 F4.2 mJy e_S3.4 [0.02/0.8] S3.4 uncertainty
48- 52 F5.2 mJy S4.6 [1/55.5] WISE 4.6 flux density
54- 57 F4.2 mJy e_S4.6 [0.03/1] S4.6 uncertainty
59- 64 F6.2 mJy S9 [65/138.2]? AKARI/IRC 9um flux density
66- 70 F5.2 mJy e_S9 [2.4/25]? S9 uncertainty
72- 77 F6.2 mJy S12 [21.7/160.3] WISE 12um flux density
79- 82 F4.2 mJy e_S12 [0.3/2.3] S12 uncertainty
84- 89 F6.2 mJy S12i [81.6/162.8]? IRAS FSC 12um flux density
91- 95 F5.2 mJy e_S12i [14.9/30.7]? S12i uncertainty
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Note (4): 2MASS magnitudes are 20mag/arcsec2 isophotal fiducial
elliptical aperture magnitudes (AB). These magnitudes represent
approximately 85% of the total flux of a galaxy (see
http://www.ipac.caltech.edu/2mass/releases/allsky/doc/sec2_3d3.html).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/47] Running sequence number
4- 9 F6.2 mJy S18 [94/344]? AKARI/IRC 18um flux density
11- 15 F5.2 mJy e_S18 [8/51]? S18 uncertainty
17- 22 F6.2 mJy S22 [34/619] WISE 22um flux density
24- 28 F5.2 mJy e_S22 [1/11] S22 uncertainty
30- 35 F6.2 mJy S25 [127/717]? IRAS FSC 25um flux density
37- 41 F5.2 mJy e_S25 [15/58]? S25 uncertainty
43- 46 F4.2 Jy S60 [0.2/5.2]? IRAS FSC 60um flux density
48- 51 F4.2 Jy e_S60 [0.04/0.4]? S60 uncertainty
53- 56 F4.2 Jy S65 [2.9/3.8]? AKARI/FIS 65um flux density
58- 61 F4.2 Jy e_S65 [0.2/0.5]? S65 uncertainty
63- 66 F4.2 Jy S90 [0.5/5.1]? AKARI/FIS 90um flux density
68- 71 F4.2 Jy e_S90 [0.02/0.3]? S90 uncertainty
73- 76 F4.2 Jy S100 [0.5/5.1]? IRAS FSC 100um flux density
78- 81 F4.2 Jy e_S100 [0.1/0.6]? S100 uncertainty
83- 86 F4.2 Jy S140 [2.8/6]? AKARI/FIS 140um flux density
88- 91 F4.2 Jy e_S140 [0.3/1.3]? S140 uncertainty
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 16-May-2014