qso absorption line - galaxy connections
DESCRIPTION
QSO Absorption Line - Galaxy Connections. Todd M. Tripp (University of Massachusetts). Above: spectrum of 4C 05.34 from Lynds (1971). QSO Absorption Line - Galaxy Connections. Part I: A brief (and semi-random) review. Above: Keck spectrum from Lu & Sargent. - PowerPoint PPT PresentationTRANSCRIPT
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QSO Absorption Line - Galaxy ConnectionsTodd 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: spectrum of 4C 05.34 from Lynds (1971)Above: Keck spectrum from Lu & Sargent
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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, A&A, 155, L8)Bergeron & Boissé (1991, A&A, 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 GalaxiesA new survey of Mg II absorbers (Bowen, Kim, Tripp et al. 2005)
Method
1. Select QSO-galaxy pairs from Sloan
2. Get galaxy redshift from HET
3. 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 GalaxiesA new survey of Mg II absorbers (Bowen, Kim, Tripp et al. 2005)
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Mg II Absorbers and Related GalaxiesA new survey of Mg II absorbers (Bowen, Kim, Tripp et al. 2005)
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Mg II Absorbers and Related GalaxiesA new survey of Mg II absorbers (Bowen, Kim, Tripp et al. 2005)
• 20 galaxies with g < 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 GalaxiesChurchill, Steidel, & Vogt (1996): “We find no correlations at the2.5 level between the measured absorption properties and galaxyproperties”
Impact parameter
High-Velocity Clouds?
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HST enabled galaxy-Lyabsorber 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 Ly 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): Ly 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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Ly EQW - impact parameter correlation
Impey, Petry & Flint (1999)Tripp, Lu, & Savage (1998)
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High spectral resolution is crucial
140 kpc230 kpc (Bechtold et al.)
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High spectral resolution is crucial
140 kpc230 kpc (Bechtold et al.)
Aracil, Tripp, Bowen, Prochaska, & Frye (2005)
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Part 2: The Missing Baryons
• Deuterium measurements: b = 0.034 (total)
• Ordinary stars in galaxies: b = 0.003 (~10%)
• Gas in galaxy clusters: b = 0.002 (~ 6%)
• Cool intergalactic gas: b = 0.008 (~24%)
• Very cold gas: b = 0.0006 (~ 2%)
• SUM of observations: b = 0.014 (~42%)
The Nearby UniverseThe Nearby Universe
The Distant UniverseThe Distant Universe
• Cool intergalactic gas: b > 0.030 (>88%)
(e.g., Persic & Salucci 1992; Fukugita, Hogan, & Peebles 1998)
c
h = 0.75WMAP: b = 0.040
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H1821+643 (Tripp et al. 1998)
PG1116+215 (Sembach et al. 2004)PG1259+593 (Richter et al. 2004)
3C 273 (based on Morris et al. 1993)
Penton, Stocke, & Shull (2004): low-z Lya forestcontains 29±4 % of the baryons
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The Search for “Warm-Hot” Intergalactic Gas
(Hydrodynamic simulation of cosmological structure from Springel et al.)
Davé, Cen et al. (2001)
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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 Features
[from Shapiro & Moore (1976: ApJ, 207, 460)]
Si IV C IV N V O VI
Steady State
4.0 5.0 6.00.001
0.01
0.1
1.0
Fra
ctio
n
Log T
Si IV C IV N V O VI
Time Dependent
4.0 5.0 6.0
Log T
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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: H1821+643
z = 0.22497
z = 0.22637
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First results on redshifted O VI absorbers(Tripp, Savage, & Jenkins 2000)
• STIS E140M spectrum of H1821+643 (zQSO = 0.297)
• Five intervening O VI doublets; one “associated” O VI system (i.e., at the QSO redshift)
• O VI dN/dz (Wr > 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 < zQSO < 0.5726)
• 44 intervening O VI absorbers
• 14 associated O VI absorbersdN/dz = 23 ± 4b (O VI) = 0.0027
Wr > 30 mÅ,z(abs) > 0.12
Danforth & Shull (2005):dN/dz = 17 ± 3b (O VI) = 0.0022
Wr > 30 mÅ,z(abs) < 0.15
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O VI discovered by Sembach et al. (2001)
Extensive galaxy redshift information available (e.g., Morris et al. 1993; Stocke et al. 2004)
Ionization & Metallicity of O VI Systems
3C 273
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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 < 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 > 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?
Morris et al. (1993)
Nearest galaxy:1.9 Mpc in projection!
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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-upsz = 0.04125: no galaxiesz = 0.05895,0.06244:purple arrowz = 0.13847: blue arrowz = 0.16548: no galaxiesz = 0.17360: red arrow
QSO(Note: additional galaxies are present atthese redshifts outsideof 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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GALEX imaging of M82 & M81(Hoopes et al. 2005, ApJ, 619, L99)
E. Burbidge et al. (2003, ApJ, 591, 690)