HST viewing of spectacular star-forming trails behind ESO 137-001

William Waldron; Ming Sun; Rongxin Luo; Sunil Laudari; Marios Chatzikos; Suresh Sivanandam; Jeffrey D.P. Kenney; Pavel Jáchym; G. Mark Voit; Megan Donahue; Matteo Fossati

doi:10.1093/mnras/stad963

HST viewing of spectacular star-forming trails behind ESO 137-001

William Waldron, Ming Sun, Rongxin Luo, Sunil Laudari, Marios Chatzikos, Suresh Sivanandam, Jeffrey D.P. Kenney, Pavel Jáchym, G. Mark Voit, Megan Donahue, Matteo Fossati

Physics And Astronomy

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1 Scopus citations

Abstract

We present the results from the HST WFC3 and ACS data on an archetypal galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H α to CO. The HST data reveal significant features indicative of RPS such as asymmetric dust distribution and surface brightness as well as many blue young star complexes in the tail. We study the correlation between the blue young star complexes from HST, H II regions from H α (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II regions is very good, while their correlation with the dense CO clumps are typically not good, presumably due in part to evolutionary effects. In comparison to the STARBURST99 + CLOUDY model, many blue regions are found to be young (<10 Myr) and the total star formation (SF) rate in the tail is 0.3–0.6 M_⊙ yr^-1 for sources measured with ages less than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace SF over at least 100 Myr and give a full picture of the recent SF history in the tail. We also demonstrate the importance of including nebular emissions and a nebular to stellar extinction correction factor when comparing the model to the broad-band data. Our work on ESO 137-001 demonstrates the importance of HST data for constraining the SF history in stripped tails.

Original language	English
Pages (from-to)	173-194
Number of pages	22
Journal	Monthly Notices of the Royal Astronomical Society
Volume	522
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stad963
State	Published - Jun 1 2023

Bibliographical note

Funding Information:
We thank useful discussion with Hugh Crowl, Claus Leitherer and Renbin Yan. We thank Nivedita Sekhar for some early work of the HST data. We thank the anonymous referee for useful comments. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-13102A and GO6-17111X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Support for this work was also provided by the NASA grants HST-GO-11683, HST-GO-12372.09, HST-GO-12756.08-A, GO4-15115X, NNX15AK29A and the NSF grant 1714764. PJ acknowledges support from the project RVO:67985815, and the project LM2023059 of the Ministry of Education, Youth and Sports of the Czech Republic.

Publisher Copyright:
© 2023 The Author(s).

Keywords

galaxies: clusters: individual: Abell 3627
galaxies: evolution
galaxies: individual: (ESO 137-001)
galaxies: star formation
galaxies: starburst

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stad963

Cite this

@article{a3f244429ae8446b9153389a0d630d1d,

title = "HST viewing of spectacular star-forming trails behind ESO 137-001",

abstract = "We present the results from the HST WFC3 and ACS data on an archetypal galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H α to CO. The HST data reveal significant features indicative of RPS such as asymmetric dust distribution and surface brightness as well as many blue young star complexes in the tail. We study the correlation between the blue young star complexes from HST, H II regions from H α (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II regions is very good, while their correlation with the dense CO clumps are typically not good, presumably due in part to evolutionary effects. In comparison to the STARBURST99 + CLOUDY model, many blue regions are found to be young (<10 Myr) and the total star formation (SF) rate in the tail is 0.3–0.6 M⊙ yr-1 for sources measured with ages less than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace SF over at least 100 Myr and give a full picture of the recent SF history in the tail. We also demonstrate the importance of including nebular emissions and a nebular to stellar extinction correction factor when comparing the model to the broad-band data. Our work on ESO 137-001 demonstrates the importance of HST data for constraining the SF history in stripped tails.",

keywords = "galaxies: clusters: individual: Abell 3627, galaxies: evolution, galaxies: individual: (ESO 137-001), galaxies: star formation, galaxies: starburst",

author = "William Waldron and Ming Sun and Rongxin Luo and Sunil Laudari and Marios Chatzikos and Suresh Sivanandam and Kenney, {Jeffrey D.P.} and Pavel J{\'a}chym and Voit, {G. Mark} and Megan Donahue and Matteo Fossati",

note = "Funding Information: We thank useful discussion with Hugh Crowl, Claus Leitherer and Renbin Yan. We thank Nivedita Sekhar for some early work of the HST data. We thank the anonymous referee for useful comments. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-13102A and GO6-17111X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Support for this work was also provided by the NASA grants HST-GO-11683, HST-GO-12372.09, HST-GO-12756.08-A, GO4-15115X, NNX15AK29A and the NSF grant 1714764. PJ acknowledges support from the project RVO:67985815, and the project LM2023059 of the Ministry of Education, Youth and Sports of the Czech Republic. Publisher Copyright: {\textcopyright} 2023 The Author(s).",

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doi = "10.1093/mnras/stad963",

language = "English",

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T1 - HST viewing of spectacular star-forming trails behind ESO 137-001

AU - Waldron, William

AU - Sun, Ming

AU - Luo, Rongxin

AU - Laudari, Sunil

AU - Chatzikos, Marios

AU - Sivanandam, Suresh

AU - Kenney, Jeffrey D.P.

AU - Jáchym, Pavel

AU - Voit, G. Mark

AU - Donahue, Megan

AU - Fossati, Matteo

N1 - Funding Information: We thank useful discussion with Hugh Crowl, Claus Leitherer and Renbin Yan. We thank Nivedita Sekhar for some early work of the HST data. We thank the anonymous referee for useful comments. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-13102A and GO6-17111X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Support for this work was also provided by the NASA grants HST-GO-11683, HST-GO-12372.09, HST-GO-12756.08-A, GO4-15115X, NNX15AK29A and the NSF grant 1714764. PJ acknowledges support from the project RVO:67985815, and the project LM2023059 of the Ministry of Education, Youth and Sports of the Czech Republic. Publisher Copyright: © 2023 The Author(s).

PY - 2023/6/1

Y1 - 2023/6/1

N2 - We present the results from the HST WFC3 and ACS data on an archetypal galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H α to CO. The HST data reveal significant features indicative of RPS such as asymmetric dust distribution and surface brightness as well as many blue young star complexes in the tail. We study the correlation between the blue young star complexes from HST, H II regions from H α (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II regions is very good, while their correlation with the dense CO clumps are typically not good, presumably due in part to evolutionary effects. In comparison to the STARBURST99 + CLOUDY model, many blue regions are found to be young (<10 Myr) and the total star formation (SF) rate in the tail is 0.3–0.6 M⊙ yr-1 for sources measured with ages less than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace SF over at least 100 Myr and give a full picture of the recent SF history in the tail. We also demonstrate the importance of including nebular emissions and a nebular to stellar extinction correction factor when comparing the model to the broad-band data. Our work on ESO 137-001 demonstrates the importance of HST data for constraining the SF history in stripped tails.

AB - We present the results from the HST WFC3 and ACS data on an archetypal galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H α to CO. The HST data reveal significant features indicative of RPS such as asymmetric dust distribution and surface brightness as well as many blue young star complexes in the tail. We study the correlation between the blue young star complexes from HST, H II regions from H α (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II regions is very good, while their correlation with the dense CO clumps are typically not good, presumably due in part to evolutionary effects. In comparison to the STARBURST99 + CLOUDY model, many blue regions are found to be young (<10 Myr) and the total star formation (SF) rate in the tail is 0.3–0.6 M⊙ yr-1 for sources measured with ages less than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace SF over at least 100 Myr and give a full picture of the recent SF history in the tail. We also demonstrate the importance of including nebular emissions and a nebular to stellar extinction correction factor when comparing the model to the broad-band data. Our work on ESO 137-001 demonstrates the importance of HST data for constraining the SF history in stripped tails.

KW - galaxies: clusters: individual: Abell 3627

KW - galaxies: evolution

KW - galaxies: individual: (ESO 137-001)

KW - galaxies: star formation

KW - galaxies: starburst

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HST viewing of spectacular star-forming trails behind ESO 137-001

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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