J/ApJ/778/128 GRB-host galaxies photometry (Perley+, 2013)
A population of massive, luminous galaxies hosting heavily dust-obscured
gamma-ray bursts: implications for the use of GRBs as tracers of cosmic star
formation.
Perley D.A., Levan A.J., Tanvir N.R., Cenko S.B., Bloom J.S., Hjorth J.,
Kruhler T., Filippenko A.V., Fruchter A., Fynbo J.P.U., Jakobsson P.,
Kalirai J., Milvang-Jensen B., Morgan A.N., Prochaska J.X., Silverman J.M.
<Astrophys. J., 778, 128 (2013)>
=2013ApJ...778..128P 2013ApJ...778..128P
ADC_Keywords: Gamma rays ; Galaxies, photometry ; Redshifts ; Extinction
Keywords: dust, extinction; galaxies: star formation; gamma-ray burst: general;
ISM: structure
Abstract:
We present observations and analysis of the host galaxies of 23
heavily dust-obscured gamma-ray bursts (GRBs) observed by the Swift
satellite during the years 2005-2009, representing all GRBs with an
unambiguous host-frame extinction of AV>1mag from this period. Deep
observations with Keck, Gemini, Very Large Telescope, Hubble Space
Telescope, and Spitzer successfully detect the host galaxies and
establish spectroscopic or photometric redshifts for all 23 events,
enabling us to provide measurements of the intrinsic host star
formation rates, stellar masses, and mean extinctions. Compared to the
hosts of unobscured GRBs at similar redshifts, we find that the hosts
of dust-obscured GRBs are (on average) more massive by about an order
of magnitude and also more rapidly star forming and dust obscured.
While this demonstrates that GRBs populate all types of star-forming
galaxies, including the most massive, luminous systems at z~2,
at redshifts below 1.5 the overall GRB population continues to show a
highly significant aversion to massive galaxies and a preference for
low-mass systems relative to what would be expected given a purely
star-formation-rate-selected galaxy sample. This supports the notion
that the GRB rate is strongly dependent on metallicity, and may
suggest that the most massive galaxies in the universe underwent a
transition in their chemical properties ∼9Gyr ago. We also conclude
that, based on the absence of unobscured GRBs in massive galaxies and
the absence of obscured GRBs in low-mass galaxies, the dust
distributions of the lowest-mass and the highest-mass galaxies are
relatively homogeneous, while intermediate-mass galaxies
(∼109M☉) have diverse internal properties.
Description:
Imaging observations of the galaxies were acquired mostly as part of
our multi-year GRB host follow-up campaign with Keck-I/LRIS.
We employed the Near-Infrared Camera (NIRC) on Keck-I during a
one-night classical run on 2009 May 31 to observe several objects.
Deep imaging observations from the Near-Infrared Imager (NIRI) on
Gemini-North were used to constrain the properties of host galaxies in
the sample.
We have obtained HST images of several of our targets, taken from a
variety of programs during Cycles 16-20.
Observations of all of our targets were carried out with the Infrared
Array Camera (IRAC) on Spitzer, mostly as part of our programs (GO
70036 and 90062, PI Perley) during Warm Mission Cycles 7 and 9.
Many hosts in this sample were observed with the VLT.
We acquired additional photometry from a variety of other literature
sources.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 76 23 GRB afterglow properties
table2.dat 88 23 Afterglow and host positions
table3.dat 57 270 Host-galaxy photometry
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See also:
J/MNRAS/426/1845 : AzTEC survey of the SHADES fields. II. (Michalowski+, 2012)
J/PASJ/63/S379 : MOIRCS Deep Survey deep and wide catalogs (Kajisawa+, 2011)
J/AJ/141/36 : GRB 080607 multi-band light curves (Perley+, 2011)
J/MNRAS/415/1479 : LESS photometric redshift survey (Wardlow+, 2011)
J/MNRAS/401/1521 : Stellar masses of Lyman break galaxies (Magdis+, 2010)
J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)
J/ApJ/701/824 : Afterglows of short & long-duration GRBs (Nysewander+, 2009)
J/ApJ/693/1484 : Early optical afterglow catalog (Cenko+, 2009)
J/ApJ/690/163 : The first Swift UV-Opt GRB afterglow catalog (Roming+, 2009)
J/A+A/504/751 : GOODS-MUSIC catalog updated version (Santini+, 2009)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/686/1209 : Optical properties of GRB afterglows (Melandri+, 2008)
J/ApJ/683/321 : Metallicities of GRB, DLA & Lyα gal. (Fynbo+, 2008)
J/AJ/133/1027 : Positions for 179 Swift X-ray afterglows (Butler+, 2007)
J/ApJ/654/L25 : Light-curve data for GRB 050319 (Huang+, 2007)
J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)
J/AJ/130/873 : Properties of BQSs in the SDSS DR3 area (Jester+, 2005)
J/AJ/127/2002 : Star Formation Rate of NFGS galaxies (Kewley+, 2004)
http://www.mpe.mpg.de/~jcg/grbgen.html : GRBs compilation
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB identifier (YYMMDDA)
9- 13 F5.3 --- z [0.3/3.1] Redshift of the GRB or host galaxy
15 A1 --- f_z [p] p: Host-galaxy photometric redshift
17- 19 I3 s T90 [12/340] T90 duration
21- 24 I4 10-10J/m2 Sg [3/1400] Gamma-ray fluence Sγ in the
Swift BAT 15-150keV band (1)
26- 29 F4.1 10+20/cm2 NH [1/84] Equivalent neutral-hydrogen column
at z=0 (2)
31- 34 F4.1 10+20/cm2 E_NH [2/18] Positive error on NH
36- 39 F4.1 10+20/cm2 e_NH [2/16] Negative error on NH
41- 44 F4.2 --- Bx [0.4/2.5] Measured X-ray spectral slope
(βX) (3)
46- 49 F4.2 --- E_Bx [0.07/0.6] Positive error on Bx
51- 54 F4.2 --- e_Bx [0.06/0.6] Negative error on Bx
56- 59 F4.2 --- Bxm [1/2.13] Minimum X-ray spectral slope (4)
61- 65 F5.2 --- Box [-0.6/0.4] Upper limit of the observed
optical-to-X-ray index βox (5)
67- 71 F5.2 mag Avl [0.5/12.3] Limiting extinction (AV in the
host frame) (6)
73 A1 --- l_Av Limit flag on Av
74- 76 F3.1 mag Av [1.3/3.7]? Measured or limiting extinction
Av,fit (7)
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Note (1): Fluence, in 10-7erg/cm2 in 15-150keV energy band, with the
exception of GRB 051022, for which the HETE WXM/FREGATE
30-400keV band is used.
Note (2): Excess X-ray absorption above the Galactic value, expressed as an
equivalent neutral-hydrogen column at z=0.
Note (3): X-ray spectral slope assumed in the afterglow extinction-fitting
analysis; measured value with uncertainties (from the automated
analysis of Butler et al. 2006ApJ...652.1390B 2006ApJ...652.1390B).
Note (4): X-ray spectral slope assumed in the afterglow extinction-fitting
analysis; "minimum" value assumed in deriving limits on extinction.
It is assumed that βX≥1.0.
Note (5): Limiting value (upper limit) of the observed optical-to-X-ray index
(corrected for Galactic extinction). The optical or NIR point after
t>1000s with the strongest constraint is chosen.
Note (6): Limiting extinction (AV in the host frame) based on analysis of
individual points relative to an extrapolation of the X-ray flux
assuming the spectral index indicated under the βX column. The
optical or NIR point after t>1000s with the strongest constraint is
shown.
Note (7): Measured or limiting extinction (AV in the host frame) based on a
fit of at least two optical/NIR points in different filters.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB identifier (YYMMDDA)
9- 10 I2 h RAh Hour of right ascension (J2000) (8)
12- 13 I2 min RAm Minute of right ascension (J2000)
15- 20 F6.3 s RAs Second of right ascension (J2000)
22 A1 --- DE- Sign of declination (J2000) (8)
23- 24 I2 deg DEd Degree of declination (J2000) (8)
26- 27 I2 arcmin DEm Arcminute of declination (J2000)
29- 33 F5.2 arcsec DEs Arcsecond of declination (J2000)
35- 38 F4.2 arcsec ePos [0.1/1.4] Position uncertainty (9)
40- 47 A8 --- Tel Telescope used for position (10)
49- 53 F5.3 mag E(B-V) [0.008/0.2] Foreground extinction from
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
55- 56 I2 h RAHh Host hour of right ascension (J2000)
58- 59 I2 min RAHm Host minute of right ascension (J2000)
61- 65 F5.2 s RAHs Host second of right ascension (J2000)
67 A1 --- DEH- Host sign of declination (J2000)
68- 69 I2 deg DEHd Host degree of declination (J2000)
71- 72 I2 arcmin DEHm Host arcminute of declination (J2000)
74- 78 F5.2 arcsec DEHs Host arcsecond of declination (J2000)
80- 82 F3.1 arcsec Rad [0.6/2]? Minimum aperture radius used for
photometry of the host galaxy
84- 88 F5.3 --- Prob [0/0.09] Random identification probability (11)
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Note (8): Best afterglow position.
Note (9): 90% confidence radius of the error circle.
Note (10): Telescope providing the most precise afterglow position:
CXO = Target-of-opportunity (ToO) observations of optically undetected
GRB afterglows acquired using the Chandra X-ray Observatory (CXO)
with ACIS-S (see section 3.8).
GROND = Gamma-Ray Burst Optical Near-IR Detector (GROND); Kruehler et al.
(2011A&A...534A.108K 2011A&A...534A.108K).
Gemini = Gemini-North/NIRI observations (see section 3.3)
KAIT = Katzman Automatic Imaging Telescope (Prochaska et al.
2009ApJ...691L..27P 2009ApJ...691L..27P)
P60 = 60 inch telescope at Palomar Observatory (Cenko+, 2009,
J/ApJ/693/1484)
PAIRITEL = Peters Automated Infrared Telescope (Bloom & Alatalo,
2005GCN..3984....1B 2005GCN..3984....1B)
UKIRT = Levan et al. 2006GCN..5461....1L 2006GCN..5461....1L
VLT = Tanvir et al. (2008MNRAS.388.1743T 2008MNRAS.388.1743T)
Note (11): Probability of inclusion of an equivalent or brighter galaxy in the
error circle due to chance
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB identifier
9- 12 A4 --- Filt Filter used in the observation
14 A1 --- l_mag Limit flag on mag
16- 20 F5.2 mag mag [16.4/28.9] Observed magnitude in Filt
22- 25 F4.2 mag e_mag [0.01/0.6]? Uncertainty in mag
27 A1 --- l_Flux Limit flag on Flux
28- 33 F6.2 uJy Flux [0.01/144.5] Observed flux density
35- 39 F5.2 uJy e_Flux [0.01/29.2]? Uncertainty in Flux
41- 55 A15 --- Tel Telescope and instrument used in observation
(Keck-I/LRIS, Spitzer/IRAC, HST, VLT, GROND,
Gemini-N, ...)
57 A1 --- Ref Reference (1)
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Note (1): All other not mentioned below are from this work.
a = Hjorth et al. 2012ApJ...756..187H 2012ApJ...756..187H
b = Wang et al. 2006GCN..4653....1W 2006GCN..4653....1W
c = Kruehler et al. 2011A&A...534A.108K 2011A&A...534A.108K
d = Jaunsen et al. 2008ApJ...681..453J 2008ApJ...681..453J
e = Hunt et al. 2011ApJ...736L..36H 2011ApJ...736L..36H
f = Svensson et al. 2012MNRAS.421...25S 2012MNRAS.421...25S
g = Hashimoto et al. 2010ApJ...719..378H 2010ApJ...719..378H
h = Malesani & Fynbo 2009GCN..9108....1M 2009GCN..9108....1M
i = Holland et al. 2010ApJ...717..223H 2010ApJ...717..223H
j = Berger et al. 2009GCN..9156....1B 2009GCN..9156....1B
k = Aoki et al. 2009GCN..9145....1A 2009GCN..9145....1A
l = Cenko et al. 2010AJ....140..224C 2010AJ....140..224C
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Apr-2015