MOLECULAR GAS ALONG A BRIGHT H α FILAMENT IN 2A 0335+096 REVEALED BY ALMA

Journal Article · Thu Dec 01 00:00:00 EST 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/832/2/148· OSTI ID:22660997

Vantyghem, A. N.; McNamara, B. R.; Hogan, M. T. ^[1]; Russell, H. R.; Fabian, A. C. ^[2]; Edge, A. C. ^[3]; Nulsen, P. E. J. ^[4]; Combes, F.; Salomé, P. ^[5]; Baum, S. A.; O’Dea, C. P. ^[6]; Donahue, M.; Voit, G. M. ^[7]; Main, R. A.; Murray, N. W.; Parrish, I. J ^[8]; O’Connell, R. W. ^[9]; Oonk, J. B. R. ^[10]; Sanders, J. S. ^[11]

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1. Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1 (Canada)
2. Institute of Astronomy, Madingley Road, Cambridge CB3 0HA (United Kingdom)
3. Department of Physics, Durham University, Durham DH1 3LE (United Kingdom)
4. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
5. LERMA, Observatoire de Paris, CNRS, UPMC, PSL Univ., 61 avenue de l’Observatoire, 75014 Paris (France)
6. Department of Physics and Astronomy, University of Manitoba, Winnipeg, MB R3T 2N2 (Canada)
7. Department of Physics and Astronomy, Michigan State University, 567 Wilson Road, East Lansing, MI 48824 (United States)
8. Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8 (Canada)
9. Department of Astronomy, University of Virginia, P.O. Box 400235, Charlottesville, VA 22904 (United States)
10. ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, NL-7990 AA Dwingeloo (Netherlands)
11. Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching (Germany)

We present ALMA CO(1–0) and CO(3–2) observations of the brightest cluster galaxy (BCG) in the 2A 0335+096 galaxy cluster ( z  = 0.0346). The total molecular gas mass of 1.13 ± 0.15 × 10{sup 9} M {sub ⊙} is divided into two components: a nuclear region and a 7 kpc long dusty filament. The central molecular gas component accounts for 3.2 ± 0.4 × 10{sup 8} M {sub ⊙} of the total supply of cold gas. Instead of forming a rotationally supported ring or disk, it is composed of two distinct, blueshifted clumps south of the nucleus and a series of low-significance redshifted clumps extending toward a nearby companion galaxy. The velocity of the redshifted clouds increases with radius to a value consistent with the companion galaxy, suggesting that an interaction between these galaxies <20 Myr ago disrupted a pre-existing molecular gas reservoir within the BCG. Most of the molecular gas, 7.8 ± 0.9 × 10{sup 8} M {sub ⊙}, is located in the filament. The CO emission is co-spatial with a 10{sup 4} K emission-line nebula and soft X-rays from 0.5 keV gas, indicating that the molecular gas has cooled out of the intracluster medium over a period of 25–100 Myr. The filament trails an X-ray cavity, suggesting that the gas has cooled from low-entropy gas that has been lifted out of the cluster core and become thermally unstable. We are unable to distinguish between inflow and outflow along the filament with the present data. Cloud velocities along the filament are consistent with gravitational free-fall near the plane of the sky, although their increasing blueshifts with radius are consistent with outflow.

• OSTI ID: 22660997
• Journal Information: Astrophysical Journal, Vol. 832, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CARBON
CARBON MONOXIDE
CLOUDS
EMISSION
ENTROPY
FILAMENTS
GALAXIES
GALAXY CLUSTERS
GALAXY NUCLEI
KEV RANGE
MASS
NEBULAE
RED SHIFT
SOFT X RADIATION