GMRT H I mapping of mid-infrared bright blue compact dwarf galaxies W1016+3754 and W2326+0608

Y. Chandola; C. W. Tsai; D. Li; C. Sengupta; Y. Z. Ma; P. Zuo

doi:10.1093/mnras/stad1618

GMRT H I mapping of mid-infrared bright blue compact dwarf galaxies W1016+3754 and W2326+0608

Y. Chandola, C. W. Tsai, D. Li, C. Sengupta, Y. Z. Ma, P. Zuo

International Centre for Radio Astronomy Research (ICRAR)

Research output: Contribution to journal › Article › peer-review

2 Citations (Scopus)

Abstract

We present the results from deep 21 cm H I mapping of two nearby Blue Compact Dwarf Galaxies (BCDGs), W1016+3754 and W2326+0608, using the Giant Metrewave Radio Telescope (GMRT). These BCDGs are bright in mid-infrared data and undergoing active star formation. With the GMRT observations, we investigate the role of cold neutral gas as the fuel resource of the current intensive star formation activity. Star formation in these galaxies is likely to be due to the infall of H I gas triggered by gravitational perturbation from nearby galaxies. The BCDG W2326+0608 and nearby galaxy SDSS J232603.86+060835.8 share a common H I envelope. We find star formation takes place in the high HI column density gas (≳10²¹ cm⁻²) regions for both BCDGs. The recent starburst and infall of metal-free gas have kept the metallicity low for the BCDG W1016+3754. The metallicity for W2326+0608 is higher, possibly due to tidal interaction with the nearby galaxy SDSS J232603.86+060835.8.

Original language	English
Pages (from-to)	3848-3862
Number of pages	15
Journal	Monthly Notices of the Royal Astronomical Society
Volume	523
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stad1618
Publication status	Published - 1 Aug 2023

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10.1093/mnras/stad1618

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@article{ea69e41d5c564aae8c01de9143db7f70,

title = "GMRT H I mapping of mid-infrared bright blue compact dwarf galaxies W1016+3754 and W2326+0608",

abstract = "We present the results from deep 21 cm H I mapping of two nearby Blue Compact Dwarf Galaxies (BCDGs), W1016+3754 and W2326+0608, using the Giant Metrewave Radio Telescope (GMRT). These BCDGs are bright in mid-infrared data and undergoing active star formation. With the GMRT observations, we investigate the role of cold neutral gas as the fuel resource of the current intensive star formation activity. Star formation in these galaxies is likely to be due to the infall of H I gas triggered by gravitational perturbation from nearby galaxies. The BCDG W2326+0608 and nearby galaxy SDSS J232603.86+060835.8 share a common H I envelope. We find star formation takes place in the high HI column density gas (≳1021 cm−2) regions for both BCDGs. The recent starburst and infall of metal-free gas have kept the metallicity low for the BCDG W1016+3754. The metallicity for W2326+0608 is higher, possibly due to tidal interaction with the nearby galaxy SDSS J232603.86+060835.8.",

keywords = "dwarf-galaxies, galaxies, star formation-radio lines, starburst-galaxies",

author = "Y. Chandola and Tsai, {C. W.} and D. Li and C. Sengupta and Ma, {Y. Z.} and P. Zuo",

note = "Funding Information: This work is supported by the National Natural Science Foundation of China (NSFC) grant no. 11988101. In this work, YC is sponsored by the Chinese Academy of Sciences visiting fellowship for researchers from developing countries, grant no. 2013FFJB0009. YC also thanks Center for Astronomical Mega-Science, CAS, for FAST distinguished young researcher fellowship (19-FAST-02) and China ministry of science and technology (MOST) for the grant no. QNJ2021061003L. YC also acknowledges support from NSFC grant no. 11550110181 and 12050410259. CWT is supported by a grant from the NSFC (grant no. 12041302). YZM is supported by the National Research Foundation of South Africa under grant no.150580, 120385 and 120378, NITheCS program {\textquoteleft}New Insights into Astrophysics and Cosmology with Theoretical Models confronting Observational Data{\textquoteright}. PZ thanks for the support from the NSFC grant no. 11903003. Funding Information: We thank the anonymous reviewer for the useful comments which helped to significantly improve the paper. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We used AIPS for data reduction which is produced and maintained by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by associated universities, Inc. CWT thanks D. Stern for attempting to get the supporting optical spectra for this paper. YC thanks Narendranath Patra for the useful discussion on data reduction. This work is supported by the National Natural Science Foundation of China (NSFC) grant no. 11988101. In this work, YC is sponsored by the Chinese Academy of Sciences visiting fellowship for researchers from developing countries, grant no. 2013FFJB0009. YC also thanks Center for Astronomical Mega-Science, CAS, for FAST distinguished young researcher fellowship (19-FAST-02) and China ministry of science and technology (MOST) for the grant no. QNJ2021061003L. YC also acknowledges support from NSFC grant no. 11550110181 and 12050410259. CWT is supported by a grant from the NSFC (grant no. 12041302). YZM is supported by the National Research Foundation of South Africa under grant no. 150580, 120385 and 120378, NITheCS program {\textquoteleft}New Insights into Astrophysics and Cosmology with Theoretical Models confronting Observational Data{\textquoteright}. PZ thanks for the support from the NSFC grant no. 11903003. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. During 2011-2018, the Arecibo Observatory (AO) was operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), in alliance with Ana G. M{\'e}ndez-Universidad Metropolitana and the Universities Space Research Association. Currently, the AO is a facility of the National Science Foundation operated under cooperative agreement (AST- 1744119) by the University of Central Florida in alliance with Universidad Ana G. Me´ndez (UAGM) and Yang Enterprises (YEI), Inc. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23. This research has made use of DSS products. The DSS was produced at the STScI under U.S. Government grant no. NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This work also made use of SDSS-III. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http: //www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michi- gan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant no. NNX09AF08G and by other grants and contracts. This work has also used different python packages e.g. NUMPY, ASTROPY, APLPY, SCIPY, and MATPLOTLIB. We thank numerous contributors to these packages. Funding Information: This work also made use of SDSS-III. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michi- gan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant no. NNX09AF08G and by other grants and contracts. This work has also used different python packages e.g. numpy, astropy, aplpy, scipy , and matplotlib . We thank numerous contributors to these packages. Funding Information: This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. During 2011-2018, the Arecibo Observatory (AO) was operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), in alliance with Ana G. M{\'e}ndez-Universidad Metropolitana and the Universities Space Research Association. Currently, the AO is a facility of the National Science Foundation operated under cooperative agreement (AST- 1744119) by the University of Central Florida in alliance with Universidad Ana G. M{\'e}ndez (UAGM) and Yang Enterprises (YEI), Inc. Funding Information: This research has made use of DSS products. The DSS was produced at the STScI under U.S. Government grant no. NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. Publisher Copyright: {\textcopyright} 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2023",

month = aug,

day = "1",

doi = "10.1093/mnras/stad1618",

language = "English",

volume = "523",

pages = "3848--3862",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - GMRT H I mapping of mid-infrared bright blue compact dwarf galaxies W1016+3754 and W2326+0608

AU - Chandola, Y.

AU - Tsai, C. W.

AU - Li, D.

AU - Sengupta, C.

AU - Ma, Y. Z.

AU - Zuo, P.

N1 - Funding Information: This work is supported by the National Natural Science Foundation of China (NSFC) grant no. 11988101. In this work, YC is sponsored by the Chinese Academy of Sciences visiting fellowship for researchers from developing countries, grant no. 2013FFJB0009. YC also thanks Center for Astronomical Mega-Science, CAS, for FAST distinguished young researcher fellowship (19-FAST-02) and China ministry of science and technology (MOST) for the grant no. QNJ2021061003L. YC also acknowledges support from NSFC grant no. 11550110181 and 12050410259. CWT is supported by a grant from the NSFC (grant no. 12041302). YZM is supported by the National Research Foundation of South Africa under grant no.150580, 120385 and 120378, NITheCS program ‘New Insights into Astrophysics and Cosmology with Theoretical Models confronting Observational Data’. PZ thanks for the support from the NSFC grant no. 11903003. Funding Information: We thank the anonymous reviewer for the useful comments which helped to significantly improve the paper. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We used AIPS for data reduction which is produced and maintained by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by associated universities, Inc. CWT thanks D. Stern for attempting to get the supporting optical spectra for this paper. YC thanks Narendranath Patra for the useful discussion on data reduction. This work is supported by the National Natural Science Foundation of China (NSFC) grant no. 11988101. In this work, YC is sponsored by the Chinese Academy of Sciences visiting fellowship for researchers from developing countries, grant no. 2013FFJB0009. YC also thanks Center for Astronomical Mega-Science, CAS, for FAST distinguished young researcher fellowship (19-FAST-02) and China ministry of science and technology (MOST) for the grant no. QNJ2021061003L. YC also acknowledges support from NSFC grant no. 11550110181 and 12050410259. CWT is supported by a grant from the NSFC (grant no. 12041302). YZM is supported by the National Research Foundation of South Africa under grant no. 150580, 120385 and 120378, NITheCS program ‘New Insights into Astrophysics and Cosmology with Theoretical Models confronting Observational Data’. PZ thanks for the support from the NSFC grant no. 11903003. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. During 2011-2018, the Arecibo Observatory (AO) was operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), in alliance with Ana G. Méndez-Universidad Metropolitana and the Universities Space Research Association. Currently, the AO is a facility of the National Science Foundation operated under cooperative agreement (AST- 1744119) by the University of Central Florida in alliance with Universidad Ana G. Me´ndez (UAGM) and Yang Enterprises (YEI), Inc. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23. This research has made use of DSS products. The DSS was produced at the STScI under U.S. Government grant no. NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This work also made use of SDSS-III. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http: //www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michi- gan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant no. NNX09AF08G and by other grants and contracts. This work has also used different python packages e.g. NUMPY, ASTROPY, APLPY, SCIPY, and MATPLOTLIB. We thank numerous contributors to these packages. Funding Information: This work also made use of SDSS-III. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michi- gan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant no. NNX09AF08G and by other grants and contracts. This work has also used different python packages e.g. numpy, astropy, aplpy, scipy , and matplotlib . We thank numerous contributors to these packages. Funding Information: This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. During 2011-2018, the Arecibo Observatory (AO) was operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), in alliance with Ana G. Méndez-Universidad Metropolitana and the Universities Space Research Association. Currently, the AO is a facility of the National Science Foundation operated under cooperative agreement (AST- 1744119) by the University of Central Florida in alliance with Universidad Ana G. Méndez (UAGM) and Yang Enterprises (YEI), Inc. Funding Information: This research has made use of DSS products. The DSS was produced at the STScI under U.S. Government grant no. NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. Publisher Copyright: © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

PY - 2023/8/1

Y1 - 2023/8/1

N2 - We present the results from deep 21 cm H I mapping of two nearby Blue Compact Dwarf Galaxies (BCDGs), W1016+3754 and W2326+0608, using the Giant Metrewave Radio Telescope (GMRT). These BCDGs are bright in mid-infrared data and undergoing active star formation. With the GMRT observations, we investigate the role of cold neutral gas as the fuel resource of the current intensive star formation activity. Star formation in these galaxies is likely to be due to the infall of H I gas triggered by gravitational perturbation from nearby galaxies. The BCDG W2326+0608 and nearby galaxy SDSS J232603.86+060835.8 share a common H I envelope. We find star formation takes place in the high HI column density gas (≳1021 cm−2) regions for both BCDGs. The recent starburst and infall of metal-free gas have kept the metallicity low for the BCDG W1016+3754. The metallicity for W2326+0608 is higher, possibly due to tidal interaction with the nearby galaxy SDSS J232603.86+060835.8.

AB - We present the results from deep 21 cm H I mapping of two nearby Blue Compact Dwarf Galaxies (BCDGs), W1016+3754 and W2326+0608, using the Giant Metrewave Radio Telescope (GMRT). These BCDGs are bright in mid-infrared data and undergoing active star formation. With the GMRT observations, we investigate the role of cold neutral gas as the fuel resource of the current intensive star formation activity. Star formation in these galaxies is likely to be due to the infall of H I gas triggered by gravitational perturbation from nearby galaxies. The BCDG W2326+0608 and nearby galaxy SDSS J232603.86+060835.8 share a common H I envelope. We find star formation takes place in the high HI column density gas (≳1021 cm−2) regions for both BCDGs. The recent starburst and infall of metal-free gas have kept the metallicity low for the BCDG W1016+3754. The metallicity for W2326+0608 is higher, possibly due to tidal interaction with the nearby galaxy SDSS J232603.86+060835.8.

KW - dwarf-galaxies

KW - galaxies

KW - star formation-radio lines

KW - starburst-galaxies

UR - http://www.scopus.com/inward/record.url?scp=85163559602&partnerID=8YFLogxK

U2 - 10.1093/mnras/stad1618

DO - 10.1093/mnras/stad1618

M3 - Article

AN - SCOPUS:85163559602

SN - 0035-8711

VL - 523

SP - 3848

EP - 3862

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

GMRT H I mapping of mid-infrared bright blue compact dwarf galaxies W1016+3754 and W2326+0608

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