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Galaxy Zoo: star-formation versus spiral arm number

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Galaxy Zoo : star-formation versus spiral arm number. / Hart, Ross E.; Bamford, Steven P.; Casteels, Kevin R. V; Kruk, Sandor J.; Lintott, Chris J.; Masters, Karen L.

In: Monthly Notices of the Royal Astronomical Society, Vol. 468, No. 2, 01.06.2017, p. 1850-1863.

Research output: Contribution to journalArticlepeer-review

Harvard

Hart, RE, Bamford, SP, Casteels, KRV, Kruk, SJ, Lintott, CJ & Masters, KL 2017, 'Galaxy Zoo: star-formation versus spiral arm number', Monthly Notices of the Royal Astronomical Society, vol. 468, no. 2, pp. 1850-1863. https://doi.org/10.1093/mnras/stx581

APA

Hart, R. E., Bamford, S. P., Casteels, K. R. V., Kruk, S. J., Lintott, C. J., & Masters, K. L. (2017). Galaxy Zoo: star-formation versus spiral arm number. Monthly Notices of the Royal Astronomical Society, 468(2), 1850-1863. https://doi.org/10.1093/mnras/stx581

Vancouver

Hart RE, Bamford SP, Casteels KRV, Kruk SJ, Lintott CJ, Masters KL. Galaxy Zoo: star-formation versus spiral arm number. Monthly Notices of the Royal Astronomical Society. 2017 Jun 1;468(2):1850-1863. https://doi.org/10.1093/mnras/stx581

Author

Hart, Ross E. ; Bamford, Steven P. ; Casteels, Kevin R. V ; Kruk, Sandor J. ; Lintott, Chris J. ; Masters, Karen L. / Galaxy Zoo : star-formation versus spiral arm number. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 468, No. 2. pp. 1850-1863.

Bibtex

@article{72158f880f7647ef82c113ed0c9e207a,
title = "Galaxy Zoo: star-formation versus spiral arm number",
abstract = "Spiral arms are common features in low-redshift disc galaxies, and are prominent sites of star formation and dust obscuration. However, spiral structure can take many forms: from galaxies displaying two strong {\textquoteleft}grand design{\textquoteright} arms to those with many {\textquoteleft}flocculent{\textquoteright} arms. We investigate how these different arm types are related to a galaxy's star formation and gas properties by making use of visual spiral arm number measurements from Galaxy Zoo 2. We combine ultraviolet and mid-infrared (MIR) photometry from GALEX and WISE to measure the rates and relative fractions of obscured and unobscured star formation in a sample of low-redshift SDSS spirals. Total star formation rate has little dependence on spiral arm multiplicity, but two-armed spirals convert their gas to stars more efficiently. We find significant differences in the fraction of obscured star formation: an additional ∼10 per cent of star formation in two-armed galaxies is identified via MIR dust emission, compared to that in many-armed galaxies. The latter are also significantly offset below the IRX–β relation for low-redshift star-forming galaxies. We present several explanations for these differences versus arm number: variations in the spatial distribution, sizes or clearing time-scales of star-forming regions (i.e. molecular clouds), or contrasting recent star formation histories.",
keywords = "astro-ph.GA, RCUK, STFC, galaxies: general, galaxies: spiral, galaxies: star formation, galaxies: structure",
author = "Hart, {Ross E.} and Bamford, {Steven P.} and Casteels, {Kevin R. V} and Kruk, {Sandor J.} and Lintott, {Chris J.} and Masters, {Karen L.}",
note = "15 pages, 13 figures, accepted for publication in MNRAS",
year = "2017",
month = jun,
day = "1",
doi = "10.1093/mnras/stx581",
language = "English",
volume = "468",
pages = "1850--1863",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

RIS

TY - JOUR

T1 - Galaxy Zoo

T2 - star-formation versus spiral arm number

AU - Hart, Ross E.

AU - Bamford, Steven P.

AU - Casteels, Kevin R. V

AU - Kruk, Sandor J.

AU - Lintott, Chris J.

AU - Masters, Karen L.

N1 - 15 pages, 13 figures, accepted for publication in MNRAS

PY - 2017/6/1

Y1 - 2017/6/1

N2 - Spiral arms are common features in low-redshift disc galaxies, and are prominent sites of star formation and dust obscuration. However, spiral structure can take many forms: from galaxies displaying two strong ‘grand design’ arms to those with many ‘flocculent’ arms. We investigate how these different arm types are related to a galaxy's star formation and gas properties by making use of visual spiral arm number measurements from Galaxy Zoo 2. We combine ultraviolet and mid-infrared (MIR) photometry from GALEX and WISE to measure the rates and relative fractions of obscured and unobscured star formation in a sample of low-redshift SDSS spirals. Total star formation rate has little dependence on spiral arm multiplicity, but two-armed spirals convert their gas to stars more efficiently. We find significant differences in the fraction of obscured star formation: an additional ∼10 per cent of star formation in two-armed galaxies is identified via MIR dust emission, compared to that in many-armed galaxies. The latter are also significantly offset below the IRX–β relation for low-redshift star-forming galaxies. We present several explanations for these differences versus arm number: variations in the spatial distribution, sizes or clearing time-scales of star-forming regions (i.e. molecular clouds), or contrasting recent star formation histories.

AB - Spiral arms are common features in low-redshift disc galaxies, and are prominent sites of star formation and dust obscuration. However, spiral structure can take many forms: from galaxies displaying two strong ‘grand design’ arms to those with many ‘flocculent’ arms. We investigate how these different arm types are related to a galaxy's star formation and gas properties by making use of visual spiral arm number measurements from Galaxy Zoo 2. We combine ultraviolet and mid-infrared (MIR) photometry from GALEX and WISE to measure the rates and relative fractions of obscured and unobscured star formation in a sample of low-redshift SDSS spirals. Total star formation rate has little dependence on spiral arm multiplicity, but two-armed spirals convert their gas to stars more efficiently. We find significant differences in the fraction of obscured star formation: an additional ∼10 per cent of star formation in two-armed galaxies is identified via MIR dust emission, compared to that in many-armed galaxies. The latter are also significantly offset below the IRX–β relation for low-redshift star-forming galaxies. We present several explanations for these differences versus arm number: variations in the spatial distribution, sizes or clearing time-scales of star-forming regions (i.e. molecular clouds), or contrasting recent star formation histories.

KW - astro-ph.GA

KW - RCUK

KW - STFC

KW - galaxies: general

KW - galaxies: spiral

KW - galaxies: star formation

KW - galaxies: structure

U2 - 10.1093/mnras/stx581

DO - 10.1093/mnras/stx581

M3 - Article

VL - 468

SP - 1850

EP - 1863

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 2

ER -

ID: 6691464