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Title: ALMA observation of the disruption of molecular gas in M87

Abstract

We present the results from Atacama Large Millimeter Array (ALMA) observations centred 40 arcsec (3 kpc in projection) south-east of the nucleus of M87. Here, we report the detection of extended CO (2–1) line emission with a total flux of (5.5 ± 0.6) × 10 -18 erg s -1 cm -2 and corresponding molecular gas mass M $$H{_2}$$=(4.7±0.4)×10 5M , assuming a Galactic CO to H 2 conversion factor. ALMA data indicate a line-of-sight velocity of -129 ± 3 km s -1, in good agreement with measurements based on the [C II] and H α+[N II] lines, and a velocity dispersion of σ = 27 ± 3 km s -1. The CO (2–1) emission originates only outside the radio lobe of the active galactic nucleus (AGN) seen in the 6 cm Very Large Array image, while the filament prolongs further inwards at other wavelengths. The molecular gas in M87 appears to be destroyed or excited by AGN activity, either by direct interaction with the radio plasma, or by the shock driven by the lobe into the X-ray emitting atmosphere. This is an important piece of the puzzle in understanding the impact of the central AGN on the amount of the coldest gas from which star formation can proceed.

Authors:
 [1];  [2];  [3];  [4];  [5];  [6]
  1. Inst. of Space and Astronautical Science (ISAS), Sagamihara, Kanagawa (Japan)
  2. Yale Univ., New Haven, CT (United States). Dept. of Physics and Yale Center for Astronomy & Astrophysics; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  3. MTA-Eotvos Lorand Univ. Lendulet, Budapest (Hungary); Masaryk Univ., Brno (Czech Republic). Dept. of Theoretical Physics and Astrophysics, Faculty of Science; Hiroshima Univ., Higashi-Hiroshima (Japan)
  4. Stanford Univ., CA (United States). KIPAC; Stanford Univ., CA (United States). Dept. of Physics
  5. Stanford Univ., CA (United States). KIPAC; Stanford Univ., CA (United States). Dept. of Physics; SLAC National Accelerator Lab., Menlo Park, CA (United States)
  6. ASTRON, Netherlands Inst. for Radio Astronomy, Dwingeloo (the Netherlands)
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE; Hungarian Academy of Sciences
OSTI Identifier:
1436082
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 475; Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: active; galaxies: clusters: intracluster medium; galaxies: individual: M87; radio lines: galaxies

Citation Formats

Simionescu, A., Tremblay, G., Werner, N., Canning, R. E. A., Allen, S. W., and Oonk, J. B. R. ALMA observation of the disruption of molecular gas in M87. United States: N. p., 2018. Web. doi:10.1093/mnras/sty047.
Simionescu, A., Tremblay, G., Werner, N., Canning, R. E. A., Allen, S. W., & Oonk, J. B. R. ALMA observation of the disruption of molecular gas in M87. United States. doi:10.1093/mnras/sty047.
Simionescu, A., Tremblay, G., Werner, N., Canning, R. E. A., Allen, S. W., and Oonk, J. B. R. Tue . "ALMA observation of the disruption of molecular gas in M87". United States. doi:10.1093/mnras/sty047. https://www.osti.gov/servlets/purl/1436082.
@article{osti_1436082,
title = {ALMA observation of the disruption of molecular gas in M87},
author = {Simionescu, A. and Tremblay, G. and Werner, N. and Canning, R. E. A. and Allen, S. W. and Oonk, J. B. R.},
abstractNote = {We present the results from Atacama Large Millimeter Array (ALMA) observations centred 40 arcsec (3 kpc in projection) south-east of the nucleus of M87. Here, we report the detection of extended CO (2–1) line emission with a total flux of (5.5 ± 0.6) × 10-18 erg s-1 cm-2 and corresponding molecular gas mass M$H{_2}$=(4.7±0.4)×105M⊙, assuming a Galactic CO to H2 conversion factor. ALMA data indicate a line-of-sight velocity of -129 ± 3 km s-1, in good agreement with measurements based on the [C II] and H α+[N II] lines, and a velocity dispersion of σ = 27 ± 3 km s-1. The CO (2–1) emission originates only outside the radio lobe of the active galactic nucleus (AGN) seen in the 6 cm Very Large Array image, while the filament prolongs further inwards at other wavelengths. The molecular gas in M87 appears to be destroyed or excited by AGN activity, either by direct interaction with the radio plasma, or by the shock driven by the lobe into the X-ray emitting atmosphere. This is an important piece of the puzzle in understanding the impact of the central AGN on the amount of the coldest gas from which star formation can proceed.},
doi = {10.1093/mnras/sty047},
journal = {Monthly Notices of the Royal Astronomical Society},
issn = {0035-8711},
number = 3,
volume = 475,
place = {United States},
year = {2018},
month = {1}
}

Journal Article:
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Cited by: 6 works
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Figures / Tables:

Figure 1 Figure 1: Continuum-subtracted CO(2–1) ALMA image of the filamentary structure located south-east of the M87 nucleus. The CO(2–1) flux is integrated along the spectral axis from -300 km s−1 to +300 km s−1 relative to the galaxy’s systemic velocity. The ALMA primary beam is indicated as a dashed white circle.more » Red contours indicate -3 (dashed), +3, and +6σ levels.« less

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    Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.