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4. Some Like it Hot: Linking Diffuse X-Ray Luminosity, Baryonic Mass, and Star Formation Rate in Compact Groups of Galaxies

Author

Desjardins, Tyler D, Gallagher, Sarah C, Hornschemeier, Ann E, Mulchaey, John S, Walker, Lisa May, Brandt, Willian N, Charlton, Jane C, Johnson, Kelsey E, and Tzanavaris, Panayiotis

Subjects
Astronomy
Abstract

We present an analysis of the diffuse X-ray emission in 19 compact groups (CGs) of galaxies observed with Chandra. The hottest, most X-ray luminous CGs agree well with the galaxy cluster X-ray scaling relations in L(x-T) and (L(x-sigma), even in CGs where the hot gas is associated with only the brightest galaxy. Using Spitzer photometry, we compute stellar masses and classify Hickson CGs 19, 22, 40, and 42, and RSCGs 32, 44, and 86 as fossil groups using a new definition for fossil systems that includes a broader range of masses. We find that CGs with total stellar and Hi masses are great than or equal to 10(sup (11.3) solar mass are often X-ray luminous, while lower-mass CGs only sometimes exhibit faint, localized X-ray emission. Additionally, we compare the diffuse X-ray luminosity against both the total UV and 24 micron star formation rates of each CG and optical colors of the most massive galaxy in each of the CGs. The most X-ray luminous CGs have the lowest star formation rates, likely because there is no cold gas available for star formation, either because the majority of the baryons in these CGs are in stars or the X-ray halo, or due togas stripping from the galaxies in CGs with hot halos. Finally, the optical colors that trace recent star formation histories of the most massive group galaxies do not correlate with the X-ray luminosities of the CGs, indicating that perhaps the current state of the X-ray halos is independent of the recent history of stellar mass assembly in the most massive galaxies.

Published
2014
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5. The Optical Green Valley Versus Mid-infrared Canyon in Compact Groups

Author

Walker, Lisa May, Butterfield, Natalie, Johnson, Kelsey, Zucker, Catherine, Gallagher, Sarah, Konstantopoulos, Iraklis, Zabludoff, Ann, Hornschemeier, Ann E, Tzanavaris, Panayiotis, and Charlton, Jane C

Subjects
Astrophysics
Abstract

Compact groups of galaxies provide conditions similar to those experienced by galaxies in the earlier universe. Recent work on compact groups has led to the discovery of a dearth of mid-infrared transition galaxies (MIRTGs) in Infrared Array Camera (3.6-8.0 micrometers) color space as well as at intermediate specific star formation rates. However, we find that in compact groups these MIRTGs have already transitioned to the optical ([g−r]) red sequence. We investigate the optical color-magnitude diagram (CMD) of 99 compact groups containing 348 galaxies and compare the optical CMD with mid-infrared (mid-IR) color space for compact group galaxies. Utilizing redshifts available from Sloan Digital Sky Survey, we identified new galaxy members for four groups. By combining optical and mid-IR data, we obtain information on both the dust and the stellar populations in compact group galaxies. We also compare with more isolated galaxies and galaxies in the Coma Cluster, which reveals that, similar to clusters, compact groups are dominated by optically red galaxies. While we find that compact group transition galaxies lie on the optical red sequence, LVL (Local Volume Legacy) + (plus) SINGS (Spitzer Infrared Nearby Galaxies Survey) mid-IR (infrared) transition galaxies span the range of optical colors. The dearth of mid-IR transition galaxies in compact groups may be due to a lack of moderately star-forming low mass galaxies; the relative lack of these galaxies could be due to their relatively small gravitational potential wells. This makes them more susceptible to this dynamic environment, thus causing them to more easily lose gas or be accreted by larger members.

Published
2013
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6. Intragroup and Galaxy-linked Diffuse X-ray Emission In Hickson Compact Groups

Author

Desjardins, Tyler D, Gallagher, Sarah C, Tzanavaris, Panayiotis, Mulchaey, John S, Brandt, William N, Charlton, Jane C, Garmire, Gordon P, Gronwall, Caryl, Cardiff, Ann, Johnson, Kelsey E, Konstantopoulos, Iraklis, S, and Zabludoff, Ann I

Subjects
Astronomy, Astrophysics
Abstract

Isolated compact groups (CGs) of galaxies present a range of dynamical states, group velocity dispersions, and galaxy morphologies with which to study galaxy evolution, particularly the properties of gas both within the galaxies and in the intragroup medium. As part of a large, multiwavelength examination of CGs, we present an archival study of diffuse X-ray emission in a subset of nine Hickson compact groups (HCGs) observed with the Chandra X-Ray Observatory. We find that seven of the groups in our sample exhibit detectable diffuse emission. However, unlike large-scale emission in galaxy clusters, the diffuse features in the majority of the detected groups are linked to the individual galaxies, in the form of both plumes and halos likely as a result of vigourous star formation or activity in the galaxy nucleus, as well as in emission from tidal features. Unlike previous studies from earlier X-ray missions, HCGs 31, 42, 59, and 92 are found to be consistent with the L(sub X-Tau) relationship from clusters within the errors, while HCGs 16 and 31 are consistent with the cluster L(sub X-sigma) relation, though this is likely coincidental given that the hot gas in these two systems is largely due to star formation. We find that L(sub X) increases with decreasing group Hi to dynamical-mass ratio with tentative evidence for a dependence in X-ray luminosity on Hi morphology whereby systems with intragroup Hi indicative of strong interactions are considerably more X-ray luminous than passively evolving groups. We also find a gap in the L(sub X) of groups as a function of the total group specific star formation rate. Our findings suggest that the hot gas in these groups is not in hydrostatic equilibrium and these systems are not low-mass analogs of rich groups or clusters, with the possible exception of HCG 62.

Published
2013
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10. The Relation between Galaxy ISM and Circumgalactic O vi Gas Kinematics Derived from Observations and ΛCDM Simulations

Author

Kacprzak, Glenn G., primary, Vander Vliet, Jacob R., additional, Nielsen, Nikole M., additional, Muzahid, Sowgat, additional, Pointon, Stephanie K., additional, Churchill, Christopher W., additional, Ceverino, Daniel, additional, Arraki, Kenz S., additional, Klypin, Anatoly, additional, Charlton, Jane C., additional, and Lewis, James, additional

Published
2019
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12. Equilibrium Slab Models of Lyman-Alpha Clouds

Author

Charlton, Jane C, Salpeter, Edwin E, and Hogan, Craig J

Subjects
Astrophysics
Abstract

We model the L(sub y(alpha)) clouds as slabs of hydrogen with an ionizing extragalactic radiation field incident from both sides. In general, the equilibrium configuration of a slab at redshift z approx. less than 5 is determined by a balance of the gas pressure, gravity (including the effects of a dark matter halo), and the pressure exerted by the inter-galactic medium, P(sub ext). These models have been used to make predictions of the number of slabs as a function of the neutral hydrogen column density, N(sub H). A break in the curve is predicted at the transition between regimes where gravity and pressure are the dominant confining forces, with a less rapid decrease at larger N(sub H). The transition from optically thin to optically thick slabs leads to a gap in the distribution, whose location is governed largely by the spectrum of ionizing radiation. There are certain parallels between lines of sight through the outer HI disk of spiral galaxy with increasing radius, and the progression from damped, to Lyman limit, to forest clouds. We discuss briefly the possibility that at least some of the observed low z forest clouds may be a separate population, associated with galaxies, as suggested by the observations of Bahcall et al. This population could dominate the forest at present if the dark matter attached to galaxies should lead to gravity confinement for this disk population, while the isolated clouds remain pressure confined. The formalism developed in this paper will allow a more detailed study. We also discuss a more general parameter study of the equilibrium configuration of slabs, including mock gravity and L(sub y(alpha)) photon trapping.

Published
1993
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14. A BARE MOLECULAR CLOUD AT z similar to 0.45

Author

Jones, Therese M., Misawa, Toru, Charlton, Jane C., Mshar, Andrew C., and Ferland, Gary J.

Subjects
quasars: absorption lines, galaxies: halos, intergalactic medium, galaxies: evolution
Abstract

Several neutral species (Mg I, Si I, Ca I, Fe I) have been detected in a weak Mg II absorption line system (W-r (2796) similar to 0.15 angstrom) at z similar to 0.45 along the sightline toward HE0001-2340. These observations require extreme physical conditions, as noted in D'Odorico. We place further constraints on the properties of this system by running a wide grid of photoionization models, determining that the absorbing cloud that produces the neutral absorption is extremely dense (similar to 100-1000 cm(-3)), cold (, The Astrophysical Journal. 715(2):1497-1507 (2010)

Published
2010

17. A survey of weak MgII absorbers at 0.4 < z < 2.4

Author

Narayanan, Anand, Misawa, Toru, Charlton, Jane C., and Kim, Tae-Sun

Subjects
galaxies : evolution, intergalactic medium, quasars : absorption lines, Astrophysics
Abstract

We present results from a survey of weak Mg II absorbers in the VLT/UVES spectra of 81 QSOs obtained from the ESO archive. In this survey, we identified 112 weak Mg II systems within the redshift interval 0.4 < z < 2.4 with 86% completeness down to a rest-frame equivalent width of W-r(2796) = 0.02 angstrom, covering a cumulative redshift path length of Delta Z similar to 77.3. From this sample, we estimate that the number of weak absorbers per unit redshift (dN/dz) increases from 1.06 +/- 0.04 at < z > = 1.9 to 1.76 +/- 0.08 at < z > = 1.2 and thereafter decreases to 1.51 +/- 0.09 at < z > = 0.9 and 1.06 +/- 0.10 at < z > = 0.6. Thus, we find evidence for an evolution in the population of weakMg II absorbers, with their number density peaking at z = 1.2. We also determine the equivalent width distribution of weak systems at < z > =0.9 and < z > = 1. 9. At 0.4 < z < 1.4, there is evidence for a turnover froma power law of the form n(Wr) proportional to W-r(-1.04) at Wr(2796) < 0.1 angstrom. This turnover is more extreme at 1.4 < z < 2.4, where the equivalent width distribution is close to an extrapolation of the exponential distribution function found for strong Mg II absorbers. Based on these results, we discuss the possibility that some fraction of weak Mg II absorbers, particularly single cloud systems, are related to satellite clouds surrounding strong Mg II systems. These structures could also be analogs to MilkyWay high-velocity clouds. In this context, the paucity of high-redshift weak Mg II absorbers is caused by a lack of isolated clouds accreting onto galaxies during that epoch., Article, The Astrophysical Journal. 660:1093-1105 (2007)

Published
2007

23. THE COS/UVES ABSORPTION SURVEY OF THE MAGELLANIC STREAM. III. IONIZATION, TOTAL MASS, AND INFLOW RATE ONTO THE MILKY WAY

Author

Fox, Andrew J., primary, Wakker, Bart P., additional, Barger, Kathleen A., additional, Hernandez, Audra K., additional, Richter, Philipp, additional, Lehner, Nicolas, additional, Bland-Hawthorn, Joss, additional, Charlton, Jane C., additional, Westmeier, Tobias, additional, Thom, Christopher, additional, Tumlinson, Jason, additional, Misawa, Toru, additional, Howk, J. Christopher, additional, Haffner, L. Matthew, additional, Ely, Justin, additional, Rodriguez-Hidalgo, Paola, additional, and Kumari, Nimisha, additional

Published
2014
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