spitzer observations of hickson compact groups of galaxies
DESCRIPTION
Spitzer Observations of Hickson Compact Groups of Galaxies. J. E. Hibbard (NRAO), with: K. Johnson (P.I., UVa), A. Heiderman (NRAO REU), S. Gallagher (UCLA), A. Hornschemeier (GSFC) & J. Charlton (PSU). Compact Groups:. Hickson 1982 Richness: N>3 with mTRANSCRIPT
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
J. E. Hibbard (NRAO), with:K. Johnson (P.I., UVa), A. Heiderman (NRAO REU), S. Gallagher (UCLA), A. Hornschemeier (GSFC) & J. Charlton (PSU)
Spitzer Observations of Hickson Compact Groups of Galaxies
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Compact Groups: • Hickson 1982
– Richness: N>3 with m<m1+3mag– Isolation: Rneighbor>3Rgroup
– Compactness: G<26 mag/arcsec2
– (selected off of red plates, so bias towards early types)• May be stage in evolution to cluster core, field
early type, “fossil group”, or “dry merger remnants” (c.f. yesterdays talk by Emanuela Pompei)
• Stay tuned to meeting - 6 more CG talks on schedule!
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Spitzer Survey of HCGs: • Kelsey Johnson (UVa) P.I.• IRAC and MIPS imaging of 12 close HCGs
spanning a range of evolutionary states• Use MIR to conduct a complete census of
activity (AGN; star formation) and dust content of HCGs
• This is VERY MUCH a work in progress! (some photometry completed yesterday). See Kelsey’s presentation & Amanda’s poster at January AAS (Washington D.C) for actual results!
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Spitzer IRAC 3.6, 4.5, 5.8, 8 m bands+ MIPS 24m
Radio --->Brent Groves, 2005
Starburst SED ModelsDust
StarsSpitzer
3.6m 8m 24m
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
3.6 m
5.8 m 8 m
4.5 m
Spitzer IRAC & MIPS Mid-IR Imaging
24 m
Mostly Stars, some PAHs Just Stars
Some Stars, mostly PAHs PAHs
Hot dust
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Nearby galaxies
Virgo
Virgo core
Huchtmeier 1997
So whats a nice radio astronomer like me involved for?
• Compact groups are deficient in HI with respect to field galaxies of the same type
Compact groups
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Verdes-Montenegro et al. 2001
Compact groupsVirgo
Coma Coma I group
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HI Deficiency:
HI properties of 324 isolated galaxies: Haynes & Giovanelli, 1984
DefHI = log[ M(HI:L)pred ] - log[ M(HI:L)obs ](positive for systems more deficient than isolated
galaxies of same type)
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005(L. Verdes-Montenegro, 2001)
• Evaluate evolution of HCGs, especially with respect to their cold gas content and proposed evolutionary scenario
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Can this help us understand “quenching” of star formation in
massive galaxies??
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
In models, continued infall slows color evolution of remnants
(Somerville 2005)
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
SAMs can reproduce observed bimodality by truncating SF when bulge gets above some
critical value
(Somerville 2005)
Mcrit~2x1010 Mo
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Spitzer IRAC 3.6m, 4.5m, 5.0m, 8.0m color images
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005(L. Verdes-Montenegro, 2001)
• Phase 1: HI in individual galaxies. – HCG 02– HCG 61 – HCG 59– HCG 19*– HCG 22*– HCG 07**
*=at least one member HIdef
**=all members HIdef
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 61 (N=3)R-band Halpha
IRAC
Log Lx<41.6
24um
X
Not HI Def
Vilchez & Iglesias-Paramo 1998
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 19 (N=3+2)
IRAC
Optical+HI
No X-ray
24um
X
Optical
AC
B
DVLA Archive
Not HI Def
*
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 22 (N=3)Optical+HI
X X
OpticalA
C
B
DE
IRAC 24um
ATCA Archive, thanks to B. Koribalski
Mulchaey et al. 2003
ROSATA=dSy2
(Log Lx=40.6)
DefHI=0.59
*
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
R-band Halpha
IRAC
IRAC+HI
Log Lx<41.7
24um
HCG 07 (N=4)
VLA Archive
Vilchez & Iglesias-Paramo 1998
DefHI=0.64
**
**
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005(L. Verdes-Montenegro, 2001)
• Phase 2: HI being tidal removed from galaxies. – HCG 31* – HCG 16*
*=at least one member HIdef
**=all members HIdef
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 16 (N=4+2)R-band Halpha
IRAC
Optical+HI
24um XMM
Verdes-Montenegro 2001Vilchez & Iglesias-Paramo 1998
A=LNRB=Sy2
C=SBNG
D=LNR
Log Lx=41.0
DefHI=0.41
***
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 31 (N=4+2)R-band Halpha
IRAC
Optical+HI
Log Lx<41.2
24um
Verdes-Montenegro 2001
DefHI=0.57
*
Vilchez & Iglesias-Paramo 1998
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005(L. Verdes-Montenegro, 2001)
• Phase 4: X-ray medium. no HI in central galaxies; deficient galaxies in the outskirts– HCG 48?– HCG 90**– HCG 62?
?=no HI map**=all members
HIdef
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Optical+HI
Mulchaey et al. 2003
HCG 90 (N=4+1)
ROSAT
IRAC A
CB
D
A=Sy2
D=LNR Log Lx=40.8
DefHI=1.4
*
*
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 42 (N=4)
IRAC
24um
A
C
B
D
Mulchaey et al. 2003
ROSAT
A=dLNR
Log Lx=41.8
E dominated
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 62 (N=4)
IRAC
A
CB
D
Chandra
Log Lx=42.9
E dominated
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
So what can we do with the MIR data?
• SEDs give dominant activity• Spatially separate SED
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG7C: Def=0.55
HCG7D Def=0.55
HCG7BDef>1.3
HCG7ADef=0.85
Def vs. MIR SEDs
PAHs
PAHs + warm dust
Stars
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Trends with MIR Colors
[4.5]-[8.0] (mag)
[3.6
]-[4.
5] (m
ag)
stars
AGN
PAHs
Blue=not HI DefRed=HI Def
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Trends with MIR-FIR Colors
[4.5]-[8.0] (mag)
[8]-[
24] (
mag
)
stars
Blue=not HI DefRed=HI Def
hot dust
cool dust
no dust
stars + cool dust
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
MIR and FIR Colors vs. DEF
[4.5]-[8.0] (mag)
[8]-[
24] (
mag
)
[8]-[
24] (
mag
)
[4.5]-[8.0] (mag)
[3.6]-[4.5] (mag)
[3.6
]-[4.
5] (m
ag)
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
SFR[24um] vs. Def
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Nuclear vs. Extranuclear MIR SEDs
• HCG 90
Mostly starlight
PAHs & Hot dust
HCG 90DDefHI>2.0
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Conclusions:
• None yet. But track down Kelsey or Amanda Heiderman at January AAS Meeting
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 02 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
IRACOptical+HI HCG 07
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 16 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 19 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 22 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 31 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 42 IRACOptical+HI
Map NotAvailable
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 48 IRACOptical+HI
Map NotAvailable
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 59 IRACOptical+HI
Map NotAvailable
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 61 IRACOptical+HI
Map NotAvailable
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 62 IRACOptical+HI
Map NotAvailable
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
HCG 90 IRACOptical+HI
J. Hibbard ESO Workshop: Groups of Galaxies Dec 5-9 2005
Project Goals• Optical images of the 12
Hickson Compact Groups (Hickson 1982) in the sample; they were chosen for this study based on distance (closest), angular extent (< 8 arcmin diameter), and membership (at least 3 galaxies with redshifts within 1000 km s-1 of the mean).
• Dotted blue lines enclose the groups with complete Spitzer data to date; the remainder will have a full suite of IRAC and MIPS (24 and 70 m) imaging by the end of Cycle 1.