Advanced search
1 file | 8.53 MB Add to list

Characterizing spiral arm and interarm star formation

Author
Organization
Abstract
Interarm star formation contributes significantly to a galaxy's star formation budget and provides an opportunity to study stellar birthplaces unperturbed by spiral arm dynamics. Using optical integral field spectroscopy of the nearby galaxy NGC 628 with VLT/MUSE, we construct Ha maps including detailed corrections for dust extinction and stellar absorption to identify 391 H II regions at 35 pc resolution over 12 kpc(2). Using tracers sensitive to the underlying gravitational potential, we associate H II regions with either arm (271) or interarm (120) environments. Using our full spectral coverage of each region, we find that most physical properties (luminosity, size, metallicity, ionization parameter) of H II regions are independent of environment. We calculate the fraction of Ha luminosity due to the background of diffuse ionized gas (DIG) contaminating each H II region, and find the DIG surface brightness to be higher within H II regions than in the surroundings, and slightly higher within arm H II regions. Use of the temperature-sensitive [S II]/Ha line ratio instead of the Ha surface brightness to identify the boundaries of H II regions does not change this result. Using the dust attenuation as a tracer of the gas, we find depletion times consistent with previous work (2 x 10(9) yr) with no differences between the arm and interarm, but this is very sensitive to the DIG correction. Unlike molecular clouds, which can be dynamically affected by the galactic environment, we see fairly consistent properties of H II regions in both arm and interarm environments. This suggests either a difference in star formation and feedback in arms or a decoupling of dense star-forming clumps from the more extended surrounding molecular gas.
Keywords
H-II REGIONS, WARM IONIZED MEDIUM, INTEGRAL FIELD SPECTROSCOPY, HUBBLE-SPACE-TELESCOPE, WHIRLPOOL SURVEY PAWS, DENSE MOLECULAR GAS, NEARBY GALAXIES, LUMINOSITY FUNCTION, FORMATION LAW, FORMATION, EFFICIENCY, galaxies: individual (NGC 628), galaxies: ISM, galaxies: spiral, galaxies: star formation, H II regions, ISM: structure

Downloads

  • Characterizing Spiral Arm and Interarm Star Formation.pdf
    • full text
    • |
    • open access
    • |
    • PDF
    • |
    • 8.53 MB

Citation

Please use this url to cite or link to this publication:

MLA
Kreckel, K., et al. “Characterizing Spiral Arm and Interarm Star Formation.” ASTROPHYSICAL JOURNAL, vol. 827, no. 2, 2016.
APA
Kreckel, K., Blanc, G., Schinnerer, E., Groves, B., Adamo, A., Hughes, A., & van der Wel, S. M. (2016). Characterizing spiral arm and interarm star formation. ASTROPHYSICAL JOURNAL, 827(2).
Chicago author-date
Kreckel, K, GA Blanc, E Schinnerer, B Groves, A Adamo, A Hughes, and Sharon Meidt van der Wel. 2016. “Characterizing Spiral Arm and Interarm Star Formation.” ASTROPHYSICAL JOURNAL 827 (2).
Chicago author-date (all authors)
Kreckel, K, GA Blanc, E Schinnerer, B Groves, A Adamo, A Hughes, and Sharon Meidt van der Wel. 2016. “Characterizing Spiral Arm and Interarm Star Formation.” ASTROPHYSICAL JOURNAL 827 (2).
Vancouver
1.
Kreckel K, Blanc G, Schinnerer E, Groves B, Adamo A, Hughes A, et al. Characterizing spiral arm and interarm star formation. ASTROPHYSICAL JOURNAL. 2016;827(2).
IEEE
[1]
K. Kreckel et al., “Characterizing spiral arm and interarm star formation,” ASTROPHYSICAL JOURNAL, vol. 827, no. 2, 2016.
@article{8622248,
  abstract     = {Interarm star formation contributes significantly to a galaxy's star formation budget and provides an opportunity to study stellar birthplaces unperturbed by spiral arm dynamics. Using optical integral field spectroscopy of the nearby galaxy NGC 628 with VLT/MUSE, we construct Ha maps including detailed corrections for dust extinction and stellar absorption to identify 391 H II regions at 35 pc resolution over 12 kpc(2). Using tracers sensitive to the underlying gravitational potential, we associate H II regions with either arm (271) or interarm (120) environments. Using our full spectral coverage of each region, we find that most physical properties (luminosity, size, metallicity, ionization parameter) of H II regions are independent of environment. We calculate the fraction of Ha luminosity due to the background of diffuse ionized gas (DIG) contaminating each H II region, and find the DIG surface brightness to be higher within H II regions than in the surroundings, and slightly higher within arm H II regions. Use of the temperature-sensitive [S II]/Ha line ratio instead of the Ha surface brightness to identify the boundaries of H II regions does not change this result. Using the dust attenuation as a tracer of the gas, we find depletion times consistent with previous work (2 x 10(9) yr) with no differences between the arm and interarm, but this is very sensitive to the DIG correction. Unlike molecular clouds, which can be dynamically affected by the galactic environment, we see fairly consistent properties of H II regions in both arm and interarm environments. This suggests either a difference in star formation and feedback in arms or a decoupling of dense star-forming clumps from the more extended surrounding molecular gas.},
  articleno    = {103},
  author       = {Kreckel, K and Blanc, GA and Schinnerer, E and Groves, B and Adamo, A and Hughes, A and van der Wel, Sharon Meidt},
  issn         = {0004-637X},
  journal      = {ASTROPHYSICAL JOURNAL},
  keywords     = {H-II REGIONS,WARM IONIZED MEDIUM,INTEGRAL FIELD SPECTROSCOPY,HUBBLE-SPACE-TELESCOPE,WHIRLPOOL SURVEY PAWS,DENSE MOLECULAR GAS,NEARBY GALAXIES,LUMINOSITY FUNCTION,FORMATION LAW,FORMATION,EFFICIENCY,galaxies: individual (NGC 628),galaxies: ISM,galaxies: spiral,galaxies: star formation,H II regions,ISM: structure},
  language     = {eng},
  number       = {2},
  pages        = {9},
  title        = {Characterizing spiral arm and interarm star formation},
  url          = {http://dx.doi.org/10.3847/0004-637X/827/2/103},
  volume       = {827},
  year         = {2016},
}

Altmetric
View in Altmetric
Web of Science
Times cited: