Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc
Abstract In this paper, we test if nearby blue spheroid (BSph) galaxies may become the progenitors of star-forming spiral galaxies or passively evolving elliptical galaxies. Our sample comprises 428 galaxies of various morphologies in the redshift range 0.002
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2018-03, Vol.475 (1), p.788-799 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Mahajan, Smriti Drinkwater, Michael J Driver, S Hopkins, A M Graham, Alister W Brough, S Brown, Michael J I Holwerda, B W Owers, Matt S Pimbblet, Kevin A |
| description | Abstract
In this paper, we test if nearby blue spheroid (BSph) galaxies may become the progenitors of star-forming spiral galaxies or passively evolving elliptical galaxies. Our sample comprises 428 galaxies of various morphologies in the redshift range 0.002 |
| doi_str_mv | 10.1093/mnras/stx3202 |
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In this paper, we test if nearby blue spheroid (BSph) galaxies may become the progenitors of star-forming spiral galaxies or passively evolving elliptical galaxies. Our sample comprises 428 galaxies of various morphologies in the redshift range 0.002 < z < 0.02 (8–87 Mpc) with panchromatic data from the Galaxy and Mass Assembly survey. We find that BSph galaxies are structurally (mean effective surface brightness, effective radius) very similar to their passively evolving red counterparts. However, their star formation and other properties such as colour, age, and metallicity are more like star-forming spirals than spheroids (ellipticals and lenticulars). We show that BSph galaxies are statistically distinguishable from other spheroids as well as spirals in the multidimensional space mapped by luminosity-weighted age, metallicity, dust mass, and specific star formation rate. We use H i data to reveal that some of the BSphs are (further) developing their discs, hence their blue colours. They may eventually become spiral galaxies – if sufficient gas accretion occurs – or more likely fade into low-mass red galaxies.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stx3202</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Accretion disks ; Assembly ; Deposition ; Elliptical galaxies ; Galactic evolution ; Luminosity ; Metallicity ; Morphology ; Red shift ; Spheroids ; Spiral galaxies ; Spirals ; Star & galaxy formation ; Star formation rate ; Stars & galaxies ; Stellar age ; Stellar evolution ; Surface brightness</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2018-03, Vol.475 (1), p.788-799</ispartof><rights>2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2018</rights><rights>2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c337t-a3e3da2d83e71ba4061601d1d736a4bc1f423174d083936dcc13724912f8aadf3</citedby><cites>FETCH-LOGICAL-c337t-a3e3da2d83e71ba4061601d1d736a4bc1f423174d083936dcc13724912f8aadf3</cites><orcidid>0000-0003-4867-0022 ; 0000-0002-9796-1363 ; 0000-0002-6954-2137</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stx3202$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Mahajan, Smriti</creatorcontrib><creatorcontrib>Drinkwater, Michael J</creatorcontrib><creatorcontrib>Driver, S</creatorcontrib><creatorcontrib>Hopkins, A M</creatorcontrib><creatorcontrib>Graham, Alister W</creatorcontrib><creatorcontrib>Brough, S</creatorcontrib><creatorcontrib>Brown, Michael J I</creatorcontrib><creatorcontrib>Holwerda, B W</creatorcontrib><creatorcontrib>Owers, Matt S</creatorcontrib><creatorcontrib>Pimbblet, Kevin A</creatorcontrib><title>Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc</title><title>Monthly notices of the Royal Astronomical Society</title><description>Abstract
In this paper, we test if nearby blue spheroid (BSph) galaxies may become the progenitors of star-forming spiral galaxies or passively evolving elliptical galaxies. Our sample comprises 428 galaxies of various morphologies in the redshift range 0.002 < z < 0.02 (8–87 Mpc) with panchromatic data from the Galaxy and Mass Assembly survey. We find that BSph galaxies are structurally (mean effective surface brightness, effective radius) very similar to their passively evolving red counterparts. However, their star formation and other properties such as colour, age, and metallicity are more like star-forming spirals than spheroids (ellipticals and lenticulars). We show that BSph galaxies are statistically distinguishable from other spheroids as well as spirals in the multidimensional space mapped by luminosity-weighted age, metallicity, dust mass, and specific star formation rate. We use H i data to reveal that some of the BSphs are (further) developing their discs, hence their blue colours. 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In this paper, we test if nearby blue spheroid (BSph) galaxies may become the progenitors of star-forming spiral galaxies or passively evolving elliptical galaxies. Our sample comprises 428 galaxies of various morphologies in the redshift range 0.002 < z < 0.02 (8–87 Mpc) with panchromatic data from the Galaxy and Mass Assembly survey. We find that BSph galaxies are structurally (mean effective surface brightness, effective radius) very similar to their passively evolving red counterparts. However, their star formation and other properties such as colour, age, and metallicity are more like star-forming spirals than spheroids (ellipticals and lenticulars). We show that BSph galaxies are statistically distinguishable from other spheroids as well as spirals in the multidimensional space mapped by luminosity-weighted age, metallicity, dust mass, and specific star formation rate. We use H i data to reveal that some of the BSphs are (further) developing their discs, hence their blue colours. They may eventually become spiral galaxies – if sufficient gas accretion occurs – or more likely fade into low-mass red galaxies.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stx3202</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0003-4867-0022</orcidid><orcidid>https://orcid.org/0000-0002-9796-1363</orcidid><orcidid>https://orcid.org/0000-0002-6954-2137</orcidid><oa>free_for_read</oa></addata></record> |
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| source | OUP_牛津大学出版社OA刊 |
| subjects | Accretion disks Assembly Deposition Elliptical galaxies Galactic evolution Luminosity Metallicity Morphology Red shift Spheroids Spiral galaxies Spirals Star & galaxy formation Star formation rate Stars & galaxies Stellar age Stellar evolution Surface brightness |
| title | Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc |
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