The Enigmatic (Almost) Dark Galaxy Coma P: The Atomic Interstellar Medium

Catherine Ball, John M. Cannon, Lukas Leisman, Elizabeth A.K. Adams, Martha P. Haynes, Gyula I.G. Józsa, Kristen McQuinn, John J. Salzer, Samantha Brunker, Riccardo Giovanelli, Gregory Hallenbeck, William Janesh, Steven Janowiecki, Michael G. Jones, Katherine L. Rhode

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

We present new high-resolution H i spectral line imaging of Coma P, the brightest H i source in the system HI 1232+20. This galaxy with extremely low surface brightness was first identified in the ALFALFA survey as an "(Almost) Dark" object: a clearly extragalactic H i source with no obvious optical counterpart in existing optical survey data (although faint ultraviolet emission was detected in archival GALEX imaging). Using a combination of data from the Westerbork Synthesis Radio Telescope and the Karl G. Jansky Very Large Array, we investigate the H i morphology and kinematics at a variety of physical scales. The H i morphology is irregular, reaching only moderate maxima in mass surface density (peak pc -2 ). Gas of lower surface brightness extends to large radial distances, with the H i diameter measured at 4.0 ±0.2 kpc inside the pc -2 level. We quantify the relationships between mass surface density of H i gas and star formation on timescales of ∼100-200 Myr as traced by GALEX far-ultraviolet emission. While Coma P has regions of dense H i gas reaching the cm -2 level typically associated with ongoing star formation, it lacks massive star formation as traced by Hα emission. The H i kinematics are extremely complex: a simple model of a rotating disk cannot describe the H i gas in Coma P. Using spatially resolved position-velocity analysis we identify two nearly perpendicular axes of projected rotation that we interpret as either the collision of two H i disks or a significant infall event. Similarly, three-dimensional modeling of the H i dynamics provides a best fit with two H i components. Coma P is just consistent (within 3σ) with the known scaling relation. It is either too large for its H i mass, has too low an H i mass for its H i size, or the two H i components artificially extend its H i size. Coma P lies within the empirical scatter at the faint end of the baryonic Tully-Fisher relation, although the complexity of the H i dynamics complicates the interpretation. Along with its large ratio of H i to stellar mass, the collective H i characteristics of Coma P make it unusual among known galaxies in the nearby universe.

Original languageEnglish (US)
Article number65
JournalAstronomical Journal
Volume155
Issue number2
DOIs
StatePublished - Feb 1 2018

Fingerprint

coma
galaxies
star formation
gas
ultraviolet emission
gases
kinematics
brightness
three-dimensional modeling
Tully-Fisher relation
axes of rotation
Very Large Array (VLA)
radio telescopes
rotating disks
stellar mass
massive stars
collision
line spectra
radio
timescale

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • galaxies: dwarf
  • galaxies: evolution
  • galaxies: individual (Coma P, AGC 229385)
  • galaxies: irregular

Cite this

Ball, C., Cannon, J. M., Leisman, L., Adams, E. A. K., Haynes, M. P., Józsa, G. I. G., ... Rhode, K. L. (2018). The Enigmatic (Almost) Dark Galaxy Coma P: The Atomic Interstellar Medium. Astronomical Journal, 155(2), [65]. https://doi.org/10.3847/1538-3881/aaa156
Ball, Catherine ; Cannon, John M. ; Leisman, Lukas ; Adams, Elizabeth A.K. ; Haynes, Martha P. ; Józsa, Gyula I.G. ; McQuinn, Kristen ; Salzer, John J. ; Brunker, Samantha ; Giovanelli, Riccardo ; Hallenbeck, Gregory ; Janesh, William ; Janowiecki, Steven ; Jones, Michael G. ; Rhode, Katherine L. / The Enigmatic (Almost) Dark Galaxy Coma P : The Atomic Interstellar Medium. In: Astronomical Journal. 2018 ; Vol. 155, No. 2.
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abstract = "We present new high-resolution H i spectral line imaging of Coma P, the brightest H i source in the system HI 1232+20. This galaxy with extremely low surface brightness was first identified in the ALFALFA survey as an {"}(Almost) Dark{"} object: a clearly extragalactic H i source with no obvious optical counterpart in existing optical survey data (although faint ultraviolet emission was detected in archival GALEX imaging). Using a combination of data from the Westerbork Synthesis Radio Telescope and the Karl G. Jansky Very Large Array, we investigate the H i morphology and kinematics at a variety of physical scales. The H i morphology is irregular, reaching only moderate maxima in mass surface density (peak pc -2 ). Gas of lower surface brightness extends to large radial distances, with the H i diameter measured at 4.0 ±0.2 kpc inside the pc -2 level. We quantify the relationships between mass surface density of H i gas and star formation on timescales of ∼100-200 Myr as traced by GALEX far-ultraviolet emission. While Coma P has regions of dense H i gas reaching the cm -2 level typically associated with ongoing star formation, it lacks massive star formation as traced by Hα emission. The H i kinematics are extremely complex: a simple model of a rotating disk cannot describe the H i gas in Coma P. Using spatially resolved position-velocity analysis we identify two nearly perpendicular axes of projected rotation that we interpret as either the collision of two H i disks or a significant infall event. Similarly, three-dimensional modeling of the H i dynamics provides a best fit with two H i components. Coma P is just consistent (within 3σ) with the known scaling relation. It is either too large for its H i mass, has too low an H i mass for its H i size, or the two H i components artificially extend its H i size. Coma P lies within the empirical scatter at the faint end of the baryonic Tully-Fisher relation, although the complexity of the H i dynamics complicates the interpretation. Along with its large ratio of H i to stellar mass, the collective H i characteristics of Coma P make it unusual among known galaxies in the nearby universe.",
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author = "Catherine Ball and Cannon, {John M.} and Lukas Leisman and Adams, {Elizabeth A.K.} and Haynes, {Martha P.} and J{\'o}zsa, {Gyula I.G.} and Kristen McQuinn and Salzer, {John J.} and Samantha Brunker and Riccardo Giovanelli and Gregory Hallenbeck and William Janesh and Steven Janowiecki and Jones, {Michael G.} and Rhode, {Katherine L.}",
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Ball, C, Cannon, JM, Leisman, L, Adams, EAK, Haynes, MP, Józsa, GIG, McQuinn, K, Salzer, JJ, Brunker, S, Giovanelli, R, Hallenbeck, G, Janesh, W, Janowiecki, S, Jones, MG & Rhode, KL 2018, 'The Enigmatic (Almost) Dark Galaxy Coma P: The Atomic Interstellar Medium', Astronomical Journal, vol. 155, no. 2, 65. https://doi.org/10.3847/1538-3881/aaa156

The Enigmatic (Almost) Dark Galaxy Coma P : The Atomic Interstellar Medium. / Ball, Catherine; Cannon, John M.; Leisman, Lukas; Adams, Elizabeth A.K.; Haynes, Martha P.; Józsa, Gyula I.G.; McQuinn, Kristen; Salzer, John J.; Brunker, Samantha; Giovanelli, Riccardo; Hallenbeck, Gregory; Janesh, William; Janowiecki, Steven; Jones, Michael G.; Rhode, Katherine L.

In: Astronomical Journal, Vol. 155, No. 2, 65, 01.02.2018.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The Enigmatic (Almost) Dark Galaxy Coma P

T2 - The Atomic Interstellar Medium

AU - Ball, Catherine

AU - Cannon, John M.

AU - Leisman, Lukas

AU - Adams, Elizabeth A.K.

AU - Haynes, Martha P.

AU - Józsa, Gyula I.G.

AU - McQuinn, Kristen

AU - Salzer, John J.

AU - Brunker, Samantha

AU - Giovanelli, Riccardo

AU - Hallenbeck, Gregory

AU - Janesh, William

AU - Janowiecki, Steven

AU - Jones, Michael G.

AU - Rhode, Katherine L.

PY - 2018/2/1

Y1 - 2018/2/1

N2 - We present new high-resolution H i spectral line imaging of Coma P, the brightest H i source in the system HI 1232+20. This galaxy with extremely low surface brightness was first identified in the ALFALFA survey as an "(Almost) Dark" object: a clearly extragalactic H i source with no obvious optical counterpart in existing optical survey data (although faint ultraviolet emission was detected in archival GALEX imaging). Using a combination of data from the Westerbork Synthesis Radio Telescope and the Karl G. Jansky Very Large Array, we investigate the H i morphology and kinematics at a variety of physical scales. The H i morphology is irregular, reaching only moderate maxima in mass surface density (peak pc -2 ). Gas of lower surface brightness extends to large radial distances, with the H i diameter measured at 4.0 ±0.2 kpc inside the pc -2 level. We quantify the relationships between mass surface density of H i gas and star formation on timescales of ∼100-200 Myr as traced by GALEX far-ultraviolet emission. While Coma P has regions of dense H i gas reaching the cm -2 level typically associated with ongoing star formation, it lacks massive star formation as traced by Hα emission. The H i kinematics are extremely complex: a simple model of a rotating disk cannot describe the H i gas in Coma P. Using spatially resolved position-velocity analysis we identify two nearly perpendicular axes of projected rotation that we interpret as either the collision of two H i disks or a significant infall event. Similarly, three-dimensional modeling of the H i dynamics provides a best fit with two H i components. Coma P is just consistent (within 3σ) with the known scaling relation. It is either too large for its H i mass, has too low an H i mass for its H i size, or the two H i components artificially extend its H i size. Coma P lies within the empirical scatter at the faint end of the baryonic Tully-Fisher relation, although the complexity of the H i dynamics complicates the interpretation. Along with its large ratio of H i to stellar mass, the collective H i characteristics of Coma P make it unusual among known galaxies in the nearby universe.

AB - We present new high-resolution H i spectral line imaging of Coma P, the brightest H i source in the system HI 1232+20. This galaxy with extremely low surface brightness was first identified in the ALFALFA survey as an "(Almost) Dark" object: a clearly extragalactic H i source with no obvious optical counterpart in existing optical survey data (although faint ultraviolet emission was detected in archival GALEX imaging). Using a combination of data from the Westerbork Synthesis Radio Telescope and the Karl G. Jansky Very Large Array, we investigate the H i morphology and kinematics at a variety of physical scales. The H i morphology is irregular, reaching only moderate maxima in mass surface density (peak pc -2 ). Gas of lower surface brightness extends to large radial distances, with the H i diameter measured at 4.0 ±0.2 kpc inside the pc -2 level. We quantify the relationships between mass surface density of H i gas and star formation on timescales of ∼100-200 Myr as traced by GALEX far-ultraviolet emission. While Coma P has regions of dense H i gas reaching the cm -2 level typically associated with ongoing star formation, it lacks massive star formation as traced by Hα emission. The H i kinematics are extremely complex: a simple model of a rotating disk cannot describe the H i gas in Coma P. Using spatially resolved position-velocity analysis we identify two nearly perpendicular axes of projected rotation that we interpret as either the collision of two H i disks or a significant infall event. Similarly, three-dimensional modeling of the H i dynamics provides a best fit with two H i components. Coma P is just consistent (within 3σ) with the known scaling relation. It is either too large for its H i mass, has too low an H i mass for its H i size, or the two H i components artificially extend its H i size. Coma P lies within the empirical scatter at the faint end of the baryonic Tully-Fisher relation, although the complexity of the H i dynamics complicates the interpretation. Along with its large ratio of H i to stellar mass, the collective H i characteristics of Coma P make it unusual among known galaxies in the nearby universe.

KW - galaxies: dwarf

KW - galaxies: evolution

KW - galaxies: individual (Coma P, AGC 229385)

KW - galaxies: irregular

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Ball C, Cannon JM, Leisman L, Adams EAK, Haynes MP, Józsa GIG et al. The Enigmatic (Almost) Dark Galaxy Coma P: The Atomic Interstellar Medium. Astronomical Journal. 2018 Feb 1;155(2). 65. https://doi.org/10.3847/1538-3881/aaa156