Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc

Smriti Mahajan; Michael J. Drinkwater; S. Driver; A. M. Hopkins; Alister W. Graham; S. Brough; Michael J. I. Brown; B. W. Holwerda; Matt S. Owers; Kevin A. Pimbblet

doi:10.1093/mnras/stx3202

Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc

Smriti Mahajan, Michael J. Drinkwater, S. Driver, A. M. Hopkins, Alister W. Graham, S. Brough, Michael J. I. Brown, B. W. Holwerda, Matt S. Owers, Kevin A. Pimbblet

School of Physics and Astronomy

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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 multi-dimensional space mapped by luminosity-weighted age, metallicity, dust mass and specific star formation rate. We use HI data to reveal that some of the BSphs are (further) developing their disks, hence their blue colours. They may eventually become spiral galaxies — if sufficient gas accretion occurs — or more likely fade into low-mass red galaxies.

Original language	English
Pages (from-to)	788-799
Journal	Monthly Notices of the Royal Astronomical Society
Volume	475
Issue number	1
Early online date	12 Dec 2017
DOIs	https://doi.org/10.1093/mnras/stx3202
Publication status	Published - 21 Mar 2018

Keywords

Galaxies: evolution
Galaxies: fundamental parameters
Galaxies: star formation
Galaxies: stellar content
Galaxies: structure

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10.1093/mnras/stx3202

Mahajan-2018-GAMA-MNRAS-788
© 2017, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stx3202
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GAMA Data Release 2
Liske, J. (Creator), Baldry, I. K. (Creator), Driver, S. P. (Creator), Tuffs, R. J. (Creator), Alpaslan, M. (Creator), Andrae, E. (Creator), Brough, S. (Creator), Cluver, M. E. (Creator), Grootes, M. W. (Creator), Gunawardhana, M. L. P. (Creator), Kelvin, L. S. (Creator), Loveday, J. (Creator), Robotham, A. S. G. (Creator), Bamford, S. P. (Creator), Bland-Hawthorn, J. (Creator), Brown, M. J. I. (Creator), Drinkwater, M. J. (Creator), Hopkins, A. M. (Creator), Meyer, M. J. (Creator), Norberg, P. (Creator), Peacock, J. A. (Creator), Agius, N. K. (Creator), Andrews, S. K. (Creator), Bauer, A. E. (Creator), Ching, J. H. Y. (Creator), Colles, M. (Creator), Conselice, C. J. (Creator), Croom, S. M. (Creator), Davies, L. J. M. (Creator), De Propris, R. (Creator), Dunne, L. (Creator), Eardley, E. M. (Creator), Ellis, S. (Creator), Foster, C. (Creator), Frenk, C. S. (Creator), Haußler, B. (Creator), Holwerda, B. W. (Creator), Howlett, C. (Creator), Ibarra, H. (Creator), Jarvis, M. J. (Creator), Jones, D. H. (Creator), Kafle, P. R. (Creator), Lacey, C. G. (Creator), Lange, R. (Creator), Lara-Ĺopez, M. A. (Creator), López-Sánchez, Á. R. (Creator), Maddox, S. (Creator), Madore, B. F. (Creator), McNaught-Roberts, T. (Creator), Moffett, A. J. (Creator), Nichol, R. C. (Creator), Owers, M. S. (Creator), Palamara, D. (Creator), Penny, S. J. (Creator), Phillipps, S. (Creator), Pimbblet, K. A. (Creator), Popescu, C. C. (Creator), Prescott, M. (Creator), Proctor, R. (Creator), Sadler, E. M. (Creator), Sansom, A. E. (Creator), Seibert, M. (Creator), Sharp, R. (Creator), Sutherland, W. (Creator), Vazquez-Mata, J. A. (Creator), van Kampen, E. (Creator), Wilkins, S. M. (Creator), Williams, R. (Creator) & Wright, A. H. (Creator), Galaxy And Mass Assembly (GAMA), 11 Sept 2015
http://www.gama-survey.org/dr2/
Dataset

Cite this

@article{4381500938234fbaab47fb1e34e81912,

title = "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 < 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 multi-dimensional space mapped by luminosity-weighted age, metallicity, dust mass and specific star formation rate. We use HI data to reveal that some of the BSphs are (further) developing their disks, hence their blue colours. They may eventually become spiral galaxies — if sufficient gas accretion occurs — or more likely fade into low-mass red galaxies.",

keywords = "Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: star formation, Galaxies: stellar content, Galaxies: structure",

author = "Smriti Mahajan and Drinkwater, {Michael J.} and S. Driver and Hopkins, {A. M.} and Graham, {Alister W.} and S. Brough and Brown, {Michael J. I.} and Holwerda, {B. W.} and Owers, {Matt S.} and Pimbblet, {Kevin A.}",

year = "2018",

month = mar,

day = "21",

doi = "10.1093/mnras/stx3202",

language = "English",

volume = "475",

pages = "788--799",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

TY - JOUR

T1 - Galaxy And Mass Assembly (GAMA)

T2 - blue spheroids within 87 Mpc

AU - Mahajan, Smriti

AU - Drinkwater, Michael J.

AU - Driver, S.

AU - Hopkins, A. M.

AU - Graham, Alister W.

AU - Brough, S.

AU - Brown, Michael J. I.

AU - Holwerda, B. W.

AU - Owers, Matt S.

AU - Pimbblet, Kevin A.

PY - 2018/3/21

Y1 - 2018/3/21

N2 - 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 multi-dimensional space mapped by luminosity-weighted age, metallicity, dust mass and specific star formation rate. We use HI data to reveal that some of the BSphs are (further) developing their disks, hence their blue colours. They may eventually become spiral galaxies — if sufficient gas accretion occurs — or more likely fade into low-mass red galaxies.

AB - 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 multi-dimensional space mapped by luminosity-weighted age, metallicity, dust mass and specific star formation rate. We use HI data to reveal that some of the BSphs are (further) developing their disks, hence their blue colours. They may eventually become spiral galaxies — if sufficient gas accretion occurs — or more likely fade into low-mass red galaxies.

KW - Galaxies: evolution

KW - Galaxies: fundamental parameters

KW - Galaxies: star formation

KW - Galaxies: stellar content

KW - Galaxies: structure

U2 - 10.1093/mnras/stx3202

DO - 10.1093/mnras/stx3202

M3 - Article

SN - 0035-8711

VL - 475

SP - 788

EP - 799

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Galaxy And Mass Assembly (GAMA): blue spheroids within 87 Mpc

Abstract

Keywords

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Datasets

GAMA Data Release 2

Cite this