The SAMI Galaxy Survey

Quenching of Star Formation in Clusters I. Transition Galaxies

Matt S. Owers, Michael J. Hudson, Kyle A. Oman, Joss Bland-Hawthorn, S. Brough, Julia J. Bryant, Luca Cortese, Warrick J. Couch, Scott M. Croom, Jesse Van De Sande, Christoph Federrath, Brent Groves, A. M. Hopkins, J. S. Lawrence, Nuria P.F. Lorente, Richard M. McDermid, Anne M. Medling, Samuel N. Richards, Nicholas Scott, Dan S. Taranu & 2 others Charlotte Welker, Sukyoung Yi

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These Hd-strong (HDS) galaxies (HDSGs) are rare, making up only ∼2% (25/1220) of galaxies with stellar mass log(MM)>10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R200 of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r200,3D cluster region within the last ∼1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster.

Original languageEnglish
Article number52
JournalAstrophysical Journal
Volume873
Issue number1
DOIs
Publication statusPublished - 2019 Jan 1

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star formation
quenching
galaxies
field of view
spectroscopy
simulation
ram
stripping
distribution
stellar mass

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Owers, M. S., Hudson, M. J., Oman, K. A., Bland-Hawthorn, J., Brough, S., Bryant, J. J., ... Yi, S. (2019). The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies. Astrophysical Journal, 873(1), [52]. https://doi.org/10.3847/1538-4357/ab0201
Owers, Matt S. ; Hudson, Michael J. ; Oman, Kyle A. ; Bland-Hawthorn, Joss ; Brough, S. ; Bryant, Julia J. ; Cortese, Luca ; Couch, Warrick J. ; Croom, Scott M. ; Sande, Jesse Van De ; Federrath, Christoph ; Groves, Brent ; Hopkins, A. M. ; Lawrence, J. S. ; Lorente, Nuria P.F. ; McDermid, Richard M. ; Medling, Anne M. ; Richards, Samuel N. ; Scott, Nicholas ; Taranu, Dan S. ; Welker, Charlotte ; Yi, Sukyoung. / The SAMI Galaxy Survey : Quenching of Star Formation in Clusters I. Transition Galaxies. In: Astrophysical Journal. 2019 ; Vol. 873, No. 1.
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abstract = "We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10{\%} of their spectra within the SAMI field of view. These Hd-strong (HDS) galaxies (HDSGs) are rare, making up only ∼2{\%} (25/1220) of galaxies with stellar mass log(MM)>10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15{\%}; 17/115) and a smaller fraction (2.0{\%}; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R200 of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r200,3D cluster region within the last ∼1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster.",
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Owers, MS, Hudson, MJ, Oman, KA, Bland-Hawthorn, J, Brough, S, Bryant, JJ, Cortese, L, Couch, WJ, Croom, SM, Sande, JVD, Federrath, C, Groves, B, Hopkins, AM, Lawrence, JS, Lorente, NPF, McDermid, RM, Medling, AM, Richards, SN, Scott, N, Taranu, DS, Welker, C & Yi, S 2019, 'The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies', Astrophysical Journal, vol. 873, no. 1, 52. https://doi.org/10.3847/1538-4357/ab0201

The SAMI Galaxy Survey : Quenching of Star Formation in Clusters I. Transition Galaxies. / Owers, Matt S.; Hudson, Michael J.; Oman, Kyle A.; Bland-Hawthorn, Joss; Brough, S.; Bryant, Julia J.; Cortese, Luca; Couch, Warrick J.; Croom, Scott M.; Sande, Jesse Van De; Federrath, Christoph; Groves, Brent; Hopkins, A. M.; Lawrence, J. S.; Lorente, Nuria P.F.; McDermid, Richard M.; Medling, Anne M.; Richards, Samuel N.; Scott, Nicholas; Taranu, Dan S.; Welker, Charlotte; Yi, Sukyoung.

In: Astrophysical Journal, Vol. 873, No. 1, 52, 01.01.2019.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - Quenching of Star Formation in Clusters I. Transition Galaxies

AU - Owers, Matt S.

AU - Hudson, Michael J.

AU - Oman, Kyle A.

AU - Bland-Hawthorn, Joss

AU - Brough, S.

AU - Bryant, Julia J.

AU - Cortese, Luca

AU - Couch, Warrick J.

AU - Croom, Scott M.

AU - Sande, Jesse Van De

AU - Federrath, Christoph

AU - Groves, Brent

AU - Hopkins, A. M.

AU - Lawrence, J. S.

AU - Lorente, Nuria P.F.

AU - McDermid, Richard M.

AU - Medling, Anne M.

AU - Richards, Samuel N.

AU - Scott, Nicholas

AU - Taranu, Dan S.

AU - Welker, Charlotte

AU - Yi, Sukyoung

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These Hd-strong (HDS) galaxies (HDSGs) are rare, making up only ∼2% (25/1220) of galaxies with stellar mass log(MM)>10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R200 of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r200,3D cluster region within the last ∼1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster.

AB - We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These Hd-strong (HDS) galaxies (HDSGs) are rare, making up only ∼2% (25/1220) of galaxies with stellar mass log(MM)>10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R200 of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r200,3D cluster region within the last ∼1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster.

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Owers MS, Hudson MJ, Oman KA, Bland-Hawthorn J, Brough S, Bryant JJ et al. The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies. Astrophysical Journal. 2019 Jan 1;873(1). 52. https://doi.org/10.3847/1538-4357/ab0201