Halos of Galaxies & Quasars Doron Chelouche (IAS)

The Gaseous Halos of Galaxies and Quasars

Doron Chelouche

Institute for Advanced Study, Princeton

and…

B. Ménard (CITA), D. Bowen (Princeton), O. Gnat (Caltech/TAU)

and many others!

•Strong MgII Absorbers

•A Proposed Model

•Quasar Halos

Out

line

Halos of Galaxies & Quasars Doron Chelouche (IAS)ob

serv

atio

ns

Bahcall & Spitzer (1969): Absorbers are related to galaxies

Halos of Galaxies & Quasars Doron Chelouche (IAS)

•Galaxies : 0.07-3L*

•Unit covering factor up to Rmax

•Rmax ~ Lα (α~0.1―0.4)

•Metalicity (~0.1 solar)

•No correlation w/galaxy inclination and or rotation

Steidel et al. (1994-1997)

Rmax

Mo & Miralda-Escude (1996)Fukugita & Peebles (2005)

obse

rvat

ions

Halos of Galaxies & Quasars Doron Chelouche (IAS)

•SDSS: 106 photometric quasars

•Several dozens of close (<100kpc) separation pairs (observed w/APO & HET)

obse

rvat

ions

Covering factor for REW>0.6A absorber

Rauch et al. (2002)

Halos of Galaxies & Quasars Doron Chelouche (IAS)

thermalcloudsvNREW

a m

odel

bnbN cloudscloudsclouds )(pc100few a~

HIHHI xnN ~

Lanzetta & Bowen 1992

adopted from Rao et al. (2006)

303.0~ cmnH

a m

odel

Halos of Galaxies & Quasars Doron Chelouche (IAS)

2.0~50

)10~()1~( 13

dzdl

kpcMsunMn

dzAREWdN

halohalo

MsunM

MsunkpcrM

halo

MgII

13

11

10~

10)200(

For an L* (MgII absorbing) galaxy @z~1:

Halos of Galaxies & Quasars Doron Chelouche (IAS)Q

uasa

rs 45

90

Halos of Galaxies & Quasars Doron Chelouche (IAS)

Christensen et al. 2006

Qua

sars

Emission line[ID]

Luminosity[erg/s]

Size (50%)[kpc]

HI Lα 1044 75

CIV λ1548 5∙1043 85

OVI λ1035 4∙1043 50

NV λ1238 2∙1043 70

CIII λ977 8∙1042 90

OVIII λ18.97 2∙1042 12

[OIII] λ5007 8∙1041 110

SiIV λ1398 5∙1041 110

HI Hβ 5∙1041 80

NIII λ1991 3∙1041 100

NeX λ12.14 5∙1039 10

HeI λ10830 1039 100

MgII λ2800 3∙1038 120

Que

stio

nsHalos of Galaxies & Quasars Doron Chelouche (IAS)

•Do MgII absorbers lie in special environments (massive halos? groups?)

•How different are quasar environments from galaxy ones

•Unification on large scales

•Implications for galaxy/quasar reionization effects?

•Studying absorbers by emission (metalicity/mass)

~10L*

~1L*~0.1L*