Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Daniel Perley (Caltech)+ the SHOALS collaboration:Antonio de Ugarte Postigo (IAA)Steve Schulze (PUC)Thomas Kruehler (ESO)Tanmoy Laskar (Harvard)Antonino Cucchiara (GSFC)Ranga Chary (Caltech)Jens Hjorth (DARK)Nial Tanvir (Leicester)Javier Gorosabel (IAA)Andrew Levan (Warwick)and many others
The Swift GRB Host The Swift GRB Host Galaxy Legacy SurveyGalaxy Legacy Survey
2014-11-12 2Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
A large sample of GRB redshifts and host properties can constrain...
The History of Cosmic Star-Formation (out to very high redshift)
The Sites of Stellar Mass Assembly (including the faintest galaxies)
Connections between the ISM and Stellar Population(dust, metallicity, kinematics vs. mass, SFR, etc.)
The Nature of the GRB Progenitor(formation conditions; single star vs. binary-channel)
GRB Hosts as a Cosmological Tool
2014-11-12 3Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Selection criteria:• Occurred between 2005-2010• Swift detected; gamma-ray fluence > 10-6 erg/cm2
• Swift slewed immediately to the position• Far from the Sun at time of explosion (afterglow easily observable)• Low Milky Way foreground extinction• No nearby bright stars• Localized within 2”
(Similar procedure to VLT R/K-band host survey; Hjorth+2012)
→ 120 Swift GRBs (out of ~950 to date), 75% with predetermined redshift (usually from afterglow.)
(Currently 90% after host galaxy observations.) Redshift range 0.03 < z < 6.3
“SHOALS”:A large, deep, unbiased multiwavelength survey to include all host galaxies of all types at all redshifts.
The Swift Host Galaxy Legacy Survey
2014-11-12 4Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
SHOALS Selection Criteria
Swift Host Galaxy Legacy Survey (PI Daniel Perley)
• Swift detected; gamma-ray fluence > 10-6 erg/cm2
• Swift slewed immediately to the position• Well-observed or at least well-observable:
(a) Autonomously triggered a 2m-class telescope, or(b) >5 hours from Sun and between 2005-2010, or(c) Satisfied TOUGH positional criteria
• Low Milky Way foreground extinction• No nearby bright foreground stars• Localized within 2”
Total w/redshift completeness All Swift bursts 855 303 35%
Jakobsson+2006 248 132 53% SHOALS 134 109 81%* TOUGH sample 69 58 84% BAT6 sample 58 53 91%
*before any additional host follow-up
2014-11-12 5Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
The Swift Host Galaxy Legacy Survey
Spitzer (3.6 μm imaging): Good stellar mass proxy
(even with no color information); Sensitive to 101 0 M⊙ galaxies
to z~5 All targets observed to deep limits
(1-6 hours/target at z>1)
VLA (3 GHz continuum): Dust-unbiased SFRs 90 hours to observe 32 targets (from overlapping TOUGH survey)
Keck, Gemini, VLT, GTC Optical/NIR imaging for full SED modeling (age, extinction, improved stellar masses) Spectroscopy to complete redshift distribution Numerous programs ongoing
2014-11-12 6Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Spitzer (3.6 μm imaging): Good stellar mass proxy
(even with no color information); Sensitive to 101 0 M⊙ galaxies
to z~5 230-hour large program to observe all SHOALS targets
(+ some others of interest) PI D. Perley
Keck, Gemini, VLT, GTC Spectroscopy to complete redshift
distribution, measure metallicities of some galaxies
Multicolor optical/NIR imaging for full SED modeling
(age, extinction, improved stellar masses) Ongoing, worldwide campaign
2014-11-12 7Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
130 GRB Host Galaxies from Spitzer
2014-11-12 8Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
130 GRB Host Galaxies from Spitzer
2014-11-12 9Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host NIR luminosities to z~6
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 10Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
108 Mo
101099 M Moo
10101 01 0 M Moo
10101 11 1 M Moo
Abs
olut
e m
agn i
tude
(A
B)
stel
lar
ma
ss →
2014-11-12 11Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
Abs
olut
e m
agn i
tude
(A
B)
Milky Way
LMC
SMC108 Mo
101099 M Moo
10101 01 0 M Moo
10101 11 1 M Moo
stel
lar
ma
ss →
2014-11-12 12Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
Milky Way
LMC
SMC
2014-11-12 13Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
100% complete above m<23.2
Milky Way
LMC
SMC
2014-11-12 14Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
97% complete above m<24.4
Milky Way
LMC
SMC
2014-11-12 15Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
Milky Way
LMC
SMC
90% complete to full survey depth90% complete to full survey depth70% of targets are detected70% of targets are detected;;all but a few nondetections have strict upper limitsall but a few nondetections have strict upper limits
2014-11-12 16Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host stellar masses to z~6
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
Milky Way
LMC
SMC
2014-11-12 17Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host redshift evolution
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
Milky Way
LMC
SMC
Median GRB host mass ~7x10Median GRB host mass ~7x1099 at z=1-4 at z=1-4
… … but less than 10but less than 1099 at z<0.5! at z<0.5!
“cosmic downsizing”, but on steroids – to be continued...
2014-11-12 18Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB host redshift evolution
z = 0 - 0.5z = 0.5-1.0 z = 1.0-1.5 z = 1.5-2.0z = 2.0-2.5 z = 2.5-3.5 z = 3.5-5.0 z > 5.0
(includes upper limits)
Absolute magnitude (AB) at λ = 3.6/(1+z)-16 -17 -18 -19 -20 -21 -22 -23 -24
107 108 109 1010 1011Stellar mass (M⊙)
2014-11-12 19Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
median mass for GRB hostsmedian mass for GRB hosts
Milky Way
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 20Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
Grey points:GOODS-N galaxies from Kajisawa+2011
median mass for GRB hostsmedian mass for GRB hosts
Milky Way
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 21Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
Grey points:GOODS-N galaxies from Kajisawa+2011
median SFR-weighted mass for galaxiesmedian SFR-weighted mass for galaxies
median mass for GRB hostsmedian mass for GRB hosts
Milky Way
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 22Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
field survey completeness limit
field survey completeness limit
median SFR-weighted mass for galaxiesmedian SFR-weighted mass for galaxiesMilky Way
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 23Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
field survey completeness limit
field survey completeness limit
median mass for median mass for m<24.25 hostsm<24.25 hosts
median SFR-weighted mass for median SFR-weighted mass for m<24.25 galaxiesm<24.25 galaxies
MW
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 24Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
field survey completeness limit
field survey completeness limit
LMC
SMC
MW
Median Median luminosities luminosities consistent at z>2consistent at z>2
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 25Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
field survey completeness limit
field survey completeness limit
Galaxy cosmic Galaxy cosmic downsizingdownsizing
GRB cosmic GRB cosmic downsizingdownsizing
LMC
SMC
MW
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 26Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
field survey completeness limit
field survey completeness limit
GRBs almost totally absent in M > 101 0 galaxies since z~1
(… but not at z~2 or z~3)
MW
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 27Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Luminosity Distribution vs. Galaxies
z < 0.5z < 0.5
z > 5.0
z = 0.5-1.0 z = 1.0-1.5 z = 1.5-2.0
z = 2.0-2.5 z = 2.5-3.5 z = 3.5-5.0
107 108 109 1010 1011 107 108 109 1010 1011 107 108 109 1010 1011 107 108 109 1010 1011
-16 -18 -20 -22 -24 -18 -20 -22 -24 -18 -20 -22 -24 -18 -20 -22 -24
SFR
-wei
ghte
d ga
laxi
es
GR
B h
osts
2014-11-12 28Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Luminosity Distribution vs. Galaxies
z < 0.5z < 0.5
z > 5.0
z = 0.5-1.0 z = 1.0-1.5 z = 1.5-2.0
z = 2.0-2.5 z = 2.5-3.5 z = 3.5-5.0
107 108 109 1010 1011 107 108 109 1010 1011 107 108 109 1010 1011 107 108 109 1010 1011
-16 -18 -20 -22 -24 -18 -20 -22 -24 -18 -20 -22 -24 -18 -20 -22 -24
GR
B h
osts
1010 4x1010 1011
SFR
-wei
ghte
d ga
laxi
es
(lum
inos
ity c
utof
f)
2014-11-12 29Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Sharp Metallicity Cutoff?
z~0.1
z~0.3
z~0.8
z~1.6
Zahid et al. 2014z~1.2(interpolated)
KK04scale
z~2
z~3
Kewley et al. 2008 Erb et al. 2006Maiolino et al. 2008,2009
2014-11-12 30Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Sharp Metallicity Cutoff?
z~0.8z~1.6
7 8 9 10 11
1.0-1.5
1.5-2.0Zahid et al. 2014
z~1.2(interpolated)
KK04scale
0.5-1.0 0.5-1.0
1010
4x10101011
2014-11-12 31Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Sharp Metallicity Cutoff?
z~0.8z~1.6
7 8 9 10 11
1.0-1.5
1.5-2.0Zahid et al. 2014
z~1.2(interpolated)
KK04scale
0.5-1.0 0.5-1.0
1010
4x10101011
2014-11-12 32Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Sharp Metallicity Cutoff?
z~0.1
z~0.3
z~0.8
z~1.6
7 8 9 10 11
1.0-1.5
1.5-2.0Zahid et al. 2014
z~1.2(interpolated)
KK04scale
0.5-1.0 0.5-1.0
1010
4x10101011
z~2
z~3
Kewley et al. 2008 Erb et al. 2006Maiolino et al. 2008,2009
2014-11-12 33Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
median mass for GRB hostsmedian mass for GRB hosts
MW
LMC
SMC
Abs
olut
e m
agn i
tude
(A
B)
2014-11-12 34Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
GRB hosts vs. SFR-selected galaxies
(unknown redshift)Redshift
Rest-frame Wavelength (μm)
median mass for GRB hostsmedian mass for GRB hosts
MW
LMC
SMC
Stifled due to metal buildup in massive galaxies
Abs
olut
e m
agn i
tude
(A
B)
galaxies dominate cosmic SFR at every epoch from 1 < z < 6But probably not at z>6; Tanvir et al. 2012
~109 - 101 1 M ⊙
2014-11-12 35Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Stellar mass and dust obscuration
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
MW
LMC
SMC
2014-11-12 36Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Stellar mass and dust obscuration
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
red: dark or dusty bursts
MW
LMC
SMC
2014-11-12 37Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Stellar mass and dust obscuration
(unknown redshift)Redshift
Abs
olut
e m
agn i
tude
(A
B)
Rest-frame Wavelength (μm)
Low-mass Low-mass galaxies are galaxies are rarely dustyrarely dusty
13/18 heavily 13/18 heavily obscuredobscured
3/32 heavily 3/32 heavily obscuredobscured
High-mass High-mass galaxies are galaxies are usually usually dustydusty
MW
LMC
SMC
2014-11-12 38Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
ConclusionsGRBs probe typical star-forming galaxies at high redshift (z>1.5)
Median host mass is ~6×109 M☉, intermediate between LMC and MW.Host mass distribution agrees with SFR-weighted galaxy population; weak dependence on environment at these redshifts.Very little evolution in host mass distribution between 1.5 < z < 5.
No large, unseen population of low-mass galaxies.Deep mass-selected surveys see most cosmic SFR out to z~6.
GRB host properties significantly diverge from cosmic SFR at z<1They strongly avoid high-mass galaxies (“cosmic downsizing on steroids”)Suggests strong suppression above ~0.5-1.0 Z☉.
Possible additional dependencies (sSFR?)
GRBs provide novel constraints on high-z dust.Low-mass galaxies contain very little dust and are optically thin;
high-mass galaxies have lots of dust with high covering fraction.No strong connection between dust and galaxy properties
outside Local Group.GRBs support a significant (but non-dominant) contribution to
cosmic SFR from ULIRGs at z>1.
2014-11-12 39Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
2014-11-12 40Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Dust and Selection Bias
Av ~ 1 magunderrepresented
Av ~ 5 magmissing completely
(Compiled from data in Kann et al. 2003 & 2010, Cenko et al. 2009, Perley et al. 2009, Greiner et al. 2011)
~20% of GRBs are systematically missing from optical afterglow searches as a result of dust.
See if adding enough of these events makes a difference!
Observed Av Observed Av distributiondistribution(optically bright events)(optically bright events)
2014-11-12 41Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Different Host MorphologiesGRBs SNe
2014-11-12 42Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Lower Host Metallicities
Graham & Fruchter 2013(Levesque+2010, Modjaz+2008) Luminosity →
Met
alli
city
→
Core-collapse supernova hosts (z<0.5):Core-collapse supernova hosts (z<0.5):Type IIType IIType Ic/blType Ic/blGRB hosts
2014-11-12 43Swift @ 10, Rome, ItalyDaniel Perley The Swift Host Galaxy Legacy Survey
Lower Host Metallicities
Graham & Fruchter 2013(Levesque+2010, Modjaz+2008) Luminosity →
Met
alli
city
→
Core-collapse supernova hosts (z<0.5):Core-collapse supernova hosts (z<0.5):Type IIType IIType Ic/blType Ic/blGRB hosts
~0.7 Z☉
GRBs “common”(~1 per 105 SN)
GRBsrare
(~1 per 106 SN)
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