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The similar stellar populations of quiescent spiral and elliptical galaxies

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Abstract
We compare the stellar population properties in the central regions of visually classified non-star-forming spiral and elliptical galaxies from Galaxy Zoo and Sloan Digital Sky Survey (SDSS) Data Release 7. The galaxies lie in the redshift range 0.04 < z < 0.1 and have stellar masses larger than log M-* = 10.4. We select only face-on spiral galaxies in order to avoid contamination by light from the disc in the SDSS fibre and enabling the robust visual identification of spiral structure. Overall, we find that galaxies with larger central stellar velocity dispersions, regardless of morphological type, have older ages, higher metallicities and an increased overabundance of alpha-elements. Age and alpha-enhancement, at fixed velocity dispersion, do not depend on morphological type. The only parameter that, at a given velocity dispersion, correlates with morphological type is metallicity, where the metallicity of the bulges of spiral galaxies is 0.07 dex higher than that of the ellipticals. However, for galaxies with a given total stellar mass, this dependence on morphology disappears. Under the assumption that, for our sample, the velocity dispersion traces the mass of the bulge alone, as opposed to the total mass (bulge+disc) of the galaxy, our results imply that the formation epoch of galaxy and the duration of its star-forming period are linked to the mass of the bulge. The extent to which metals are retained within the galaxy, and not removed as a result of outflows, is determined by the total mass of the galaxy.
Keywords
DIGITAL-SKY-SURVEY, STAR-FORMATION HISTORIES, LINE-STRENGTH MAPS, 7TH, DATA RELEASE, SIMILAR-TO 1, SAURON PROJECT, FUNDAMENTAL PLANE, RED, SEQUENCE, LENTICULAR GALAXIES, LOCAL UNIVERSE, galaxies: bulges, galaxies: general, galaxies: spiral, galaxies: statistics

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Chicago
Robaina, Aday R, Ben Hoyle, Anna Gallazzi, Raul Jimenez, Arjen van der Wel, and Licia Verde. 2012. “The Similar Stellar Populations of Quiescent Spiral and Elliptical Galaxies.” Monthly Notices of the Royal Astronomical Society 427 (4): 3006–3015.
APA
Robaina, A. R., Hoyle, B., Gallazzi, A., Jimenez, R., van der Wel, A., & Verde, L. (2012). The similar stellar populations of quiescent spiral and elliptical galaxies. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 427(4), 3006–3015.
Vancouver
1.
Robaina AR, Hoyle B, Gallazzi A, Jimenez R, van der Wel A, Verde L. The similar stellar populations of quiescent spiral and elliptical galaxies. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 2012;427(4):3006–15.
MLA
Robaina, Aday R, Ben Hoyle, Anna Gallazzi, et al. “The Similar Stellar Populations of Quiescent Spiral and Elliptical Galaxies.” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 427.4 (2012): 3006–3015. Print.
@article{8573752,
  abstract     = {We compare the stellar population properties in the central regions of visually classified non-star-forming spiral and elliptical galaxies from Galaxy Zoo and Sloan Digital Sky Survey (SDSS) Data Release 7. The galaxies lie in the redshift range 0.04 < z < 0.1 and have stellar masses larger than log M-* = 10.4. We select only face-on spiral galaxies in order to avoid contamination by light from the disc in the SDSS fibre and enabling the robust visual identification of spiral structure. Overall, we find that galaxies with larger central stellar velocity dispersions, regardless of morphological type, have older ages, higher metallicities and an increased overabundance of alpha-elements. Age and alpha-enhancement, at fixed velocity dispersion, do not depend on morphological type. The only parameter that, at a given velocity dispersion, correlates with morphological type is metallicity, where the metallicity of the bulges of spiral galaxies is 0.07 dex higher than that of the ellipticals. However, for galaxies with a given total stellar mass, this dependence on morphology disappears. Under the assumption that, for our sample, the velocity dispersion traces the mass of the bulge alone, as opposed to the total mass (bulge+disc) of the galaxy, our results imply that the formation epoch of galaxy and the duration of its star-forming period are linked to the mass of the bulge. The extent to which metals are retained within the galaxy, and not removed as a result of outflows, is determined by the total mass of the galaxy.},
  author       = {Robaina, Aday R and Hoyle, Ben and Gallazzi, Anna and Jimenez, Raul and van der Wel, Arjen and Verde, Licia},
  issn         = {0035-8711},
  journal      = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
  keywords     = {DIGITAL-SKY-SURVEY,STAR-FORMATION HISTORIES,LINE-STRENGTH MAPS,7TH,DATA RELEASE,SIMILAR-TO 1,SAURON PROJECT,FUNDAMENTAL PLANE,RED,SEQUENCE,LENTICULAR GALAXIES,LOCAL UNIVERSE,galaxies: bulges,galaxies: general,galaxies: spiral,galaxies: statistics},
  language     = {eng},
  number       = {4},
  pages        = {3006--3015},
  title        = {The similar stellar populations of quiescent spiral and elliptical galaxies},
  url          = {http://dx.doi.org/10.1111/j.1365-2966.2012.21804.x},
  volume       = {427},
  year         = {2012},
}

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