QSO Absorption Line Galaxy Connections

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QSO Absorption Line - Galaxy Connections

• Todd M. Tripp
• (University of Massachusetts)

Above spectrum of 4C 05.34 from Lynds (1971)
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QSO Absorption Line - Galaxy Connections

• Part I
• A brief (and semi-random) review...

Above Keck spectrum from Lu Sargent
Above spectrum of 4C 05.34 from Lynds (1971)
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Mg II Absorbers and Related Galaxies
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Mg II Absorbers and Related Galaxies
Many Mg II-galaxy studies followed, e.g.,
Bergeron (1986, AA, 155, L8) Bergeron Boissé
(1991, AA, 243, 344) Yanny York (1992, ApJ,
391, 569) Bechtold Ellingson (1992, ApJ, 396,
20) Steidel, Dickenson, Persson (1994, ApJ,
437, L75) Bowen, Blades, Pettini (1995, ApJ,
448, 662) Churchill, Steidel, Vogt (1996, ApJ,
471, 164)
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Mg II Absorbers and Related Galaxies
Steidel, Dickenson, Persson (1994)

• Starting with known Mg II absorbers, obtained
  imaging spectroscopic galaxy redshifts
• 58 galaxies from 48 sight lines
• We have been able to identify the absorbing
  galaxy in every line of sight... 70 of the
  galaxies have been confirmed spectroscopically...
  remaining 30 have clear candidate
• Galaxies at distances from the line of sight
  consistent with the absorbers but not producing
  detectable absorption are very rare...

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Mg II Absorbers and Related Galaxies
A new survey of Mg II absorbers (Bowen, Kim,
Tripp et al. 2005)
Method

• Select QSO-galaxy pairs from Sloan
• Get galaxy redshift from HET
• Get QSO spectrum from MMT

This is the antithesis of most previous
work galaxy redshift was measured before the
QSO was observed.
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Mg II Absorbers and Related Galaxies
A new survey of Mg II absorbers (Bowen, Kim,
Tripp et al. 2005)
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Mg II Absorbers and Related Galaxies
A new survey of Mg II absorbers (Bowen, Kim,
Tripp et al. 2005)
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Mg II Absorbers and Related Galaxies
A new survey of Mg II absorbers (Bowen, Kim,
Tripp et al. 2005)

• 20 galaxies with g lt 20
• All within 60 kpc of the QSO sight line
• Luminosities range from 0.3L to 5L
• 50 of these galaxies show no Mg II absorption,
  contrary to expectations

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Mg II Absorbers and Related Galaxies
Churchill, Steidel, Vogt (1996) We find no
correlations at the 2.5s level between the
measured absorption properties and
galaxy properties
High-Velocity Clouds?
Impact parameter
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HST enabled galaxy-Lya absorber relationship
studies...
e.g., Bahcall et al. (1991), Spinrad et al. (1991)
(above spectrum from Jannuzi et al. 1998)
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Some early HST spectra were sensitive, but...
Tripp, Lu, and Savage (1998)
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Early question do Lya lines arise in halos of
individual galaxies or the intergalactic medium?

• Lanzetta et al. (1995), Chen et al. (1998, 2001)
  Lya lines are due to 200 kpc gaseous halos
  surrounding individual galaxies
• Morris et al. (1993), Stocke et al. (1995), Bowen
  et al. (1996), Le Brun et al. (1997), Tripp et
  al. (1998), Impey et al. (1999), Bowen et al.
  (2002) Lya lines are strongly correlated with
  galaxies, but a substantial fraction of the
  clouds are not connected to individual galaxies
  some are in voids

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Lya EQW - impact parameter correlation
Impey, Petry Flint (1999)
Tripp, Lu, Savage (1998)
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High spectral resolution is crucial
140 kpc
(Bechtold et al.)
230 kpc
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High spectral resolution is crucial
140 kpc
(Bechtold et al.)
230 kpc
Aracil, Tripp, Bowen, Prochaska, Frye (2005)
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Part 2 The Missing Baryons
W r/rc h 0.75
WMAP Wb 0.040
The Nearby Universe

• Deuterium measurements Wb 0.034 (total)
• Ordinary stars in galaxies Wb 0.003 (10)
• Gas in galaxy clusters Wb 0.002 ( 6)
• Cool intergalactic gas Wb 0.008 (24)
• Very cold gas Wb 0.0006 ( 2)
• SUM of observations Wb 0.014 (42)

The Distant Universe

• Cool intergalactic gas Wb gt 0.030 (gt88)

(e.g., Persic Salucci 1992 Fukugita, Hogan,
Peebles 1998)
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Penton, Stocke, Shull (2004) low-z Lya
forest contains 294 of the baryons
PG1259593 (Richter et al. 2004)
PG1116215 (Sembach et al. 2004)
H1821643 (Tripp et al. 1998)
3C 273 (based on Morris et al. 1993)
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The Search for Warm-Hot Intergalactic Gas
Davé, Cen et al. (2001)
(Hydrodynamic simulation of cosmological
structure from Springel et al.)
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Motivation Galactic Winds and Feedback
WIYN HST image of M82 (Gallagher et al.)
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Ionization Fractions for Li-like ions that have
Strong UV Featuresfrom Shapiro Moore (1976
ApJ, 207, 460)
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Tripp, Savage, Jenkins (2000) Oegerle, Tripp,
Sembach et al. (2000) Tripp, Giroux, Stocke,
Tumlinson, Oegerle (2001) Tripp Davé (2001)
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Sample STIS data at full resolution H1821643
z 0.22637
z 0.22497
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First results on redshifted O VI
absorbers(Tripp, Savage, Jenkins 2000)

• STIS E140M spectrum of H1821643 (zQSO 0.297)
• Five intervening O VI doublets one associated
  O VI system (i.e., at the QSO redshift)

• O VI dN/dz (Wr gt 30 mÅ) 48 (46,-25)
• ?b (O VI) 0.004 (0.004,-0.002)

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O VI survey results w/ good statistics

• Sixteen QSOs observed with STIS E140M, (0.1583 lt
  zQSO lt 0.5726)
• 44 intervening O VI absorbers
• 14 associated O VI absorbers

dN/dz 23 4 ?b (O VI) 0.0027
Wr gt 30 mÅ, z(abs) gt 0.12
Danforth Shull (2005)
dN/dz 17 3 ?b (O VI) 0.0022
Wr gt 30 mÅ, z(abs) lt 0.15
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Ionization Metallicity of O VI Systems
3C 273
O VI discovered by Sembach et al. (2001)
Extensive galaxy redshift information available
(e.g., Morris et al. 1993 Stocke et al. 2004)
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O VI at z 0.12005 toward 3C 273

• Narrow H I lines, well-aligned with O VI
• Only O VI and C III (e.g., no Si III or Si IV)
• Apparently very simple component structure
• H I line width implies that T lt 30,000 K

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O VI at z 0.12005 photoionized,
high-metallicity gas

• Z 0.6 Z(solar)
• nH 7 x 10-6 cm-3
• LOS thickness 20 kpc
• f(H I) 8 x 10-5
• f(O VI) 0.19
• Thermal pressure 1 cm-3 K
• Gas mass gt 106 M?

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First detection of intervening Ne VIII Hot gas,
no doubt about it!
(Savage et al. 2005, ApJ, in press,
astro-ph/0503051)

• Multiphase, multicomponent absorber
• Ly? - Ly?
• Warm, photoionized phase C III, O III, N III, Si
  III, O IV, S VI
• Warm ionized phase M/H -0.5
• Hot phase O VI and Ne VIII
• Hot phase consistent with collisional ionization
  eq. at T 6 x 105 K

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Nearby galaxies?
Nearest galaxy 1.9 Mpc in projection!
Morris et al. (1993)
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Sembach, Tripp, Savage, Richter (2004)
Redshift papers Tripp et al. (1998) Aracil et
al. (2005)
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O VI-galaxy match-ups z 0.04125 no galaxies z
0.05895,0.06244 purple arrow z 0.13847 blue
arrow z 0.16548 no galaxies z 0.17360 red
arrow
QSO
(Note additional galaxies are present at these
redshifts outside of this field of view)
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Broad Lyman alpha lines
Tripp et al. (2001) Bowen et al. (2002) Richter
et al. (2004) Sembach et al. (2004) Williger et
al. (2004)
b
log N(H I)
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Talk Summary

• New Mg II study 50 of galaxies do not have
  associated Mg II in new study
• Lya lines a variety of origins, kinematics
• Statistics and baryonic content of O VI
  absorbers consistent with first results. dN/dz
  23/-4, 5 of the baryons (or more) here
• Ionization Metallicity some photoionized, some
  collisionally ionized, many are multiphase. Wide
  range of metallicities.
• Broad Lyman alpha lines possibly also reveal
  warm-hot IGM
• Galaxies/environment strongly correlated with
  galaxies but with various origins, some
  individual galaxies, some in more remote
  locations

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E. Burbidge et al. (2003, ApJ, 591, 690)
GALEX imaging of M82 M81 (Hoopes et al. 2005,
ApJ, 619, L99)