H i-MaNGA: tracing the physics of the neutral and ionized ISM with the second data release
H i-MaNGA: tracing the physics of the neutral and ionized ISM with the second data release
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Häi-MaNGA：通过第二次数据发布追踪中性和电离 ISM 的物理特性
DOI：
10.1093/mnras/stab566
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发表时间：
2021-01
影响因子：
4.8
通讯作者：
Wiphu Rujopak
中科院分区：
文献类型：
--
作者：
David V Stark;Karen L Masters;Vladimir Avila-Reese;Rogemar Riffel;Rogerio Riffel;Nicholas Fraser Boardman;Zheng Zheng;Anne-Marie Weijmans;Sean Dillon;Catherine Fielder;Daniel Finnegan;Patricia Fofie;Julian Goddy;Emily Harrington;Zachary Pace;Wiphu Rujopak
ABSTRACT. We present the second data release for the H i-MaNGA programme of H i follow-up observations for the SDSS-IV MaNGA survey. This release contains measurements for 3669 unique galaxies, combining 2108 Green Bank Telescope observations with an updated crossmatch of the MaNGA sample with the ALFALFA survey. We combine these data with MaNGA spectroscopic measurements to examine relationships between H i-to-stellar mass ratio (${rm M_{H, {small I}}/{M_}}$) and average ISM/star formation properties probed by optical emission lines. ${rm M_{H, {small I}}/{M_}}$ is very weakly correlated with the equivalent width of H α, implying a loose connection between the instantaneous star formation rate and the H i reservoir, although the link between ${rm M_{H, {small I}}/{M_}}$ and star formation strengthens when averaged even over only moderate time-scales (∼30 Myr). Galaxies with elevated H i depletion times have enhanced [O i]/H α and depressed H α surface brightness, consistent with more H i residing in a diffuse and/or shock-heated phase that is less capable of condensing into molecular clouds. Of all optical lines, ${rm M_{H, {small I}}/{M_}}$ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between ${rm M_{H, {small I}}/{M_}}$ and gas-phase metallicity. Residuals in the ${rm M_{H, {small I}}/{M_}}$−EW(O) relation are again correlated with [O i]/H α and H α surface brightness, suggesting they are also driven by variations in the fraction of diffuse and/or shock-heated gas. We recover the strong anticorrelation between ${rm M_{H, {small I}}/{M_}}$ and gas-phase metallicity seen in previous studies. We also find a relationship between ${rm M_{H, {small I}}/{M_}}$ and [O i]6302/H α, suggesting that higher fractions of diffuse and/or shock-heated gas are more prevalent in gas-rich galaxies.
ABSTRACT. We present the second data release for the H i-MaNGA programme of H i follow-up observations for the SDSS-IV MaNGA survey. This release contains measurements for 3669 unique galaxies, combining 2108 Green Bank Telescope observations with an updated crossmatch of the MaNGA sample with the ALFALFA survey. We combine these data with MaNGA spectroscopic measurements to examine relationships between H i-to-stellar mass ratio (${rm M_{H, {small I}}/{M_}}$) and average ISM/star formation properties probed by optical emission lines. ${rm M_{H, {small I}}/{M_}}$ is very weakly correlated with the equivalent width of H α, implying a loose connection between the instantaneous star formation rate and the H i reservoir, although the link between ${rm M_{H, {small I}}/{M_}}$ and star formation strengthens when averaged even over only moderate time-scales (∼30 Myr). Galaxies with elevated H i depletion times have enhanced [O i]/H α and depressed H α surface brightness, consistent with more H i residing in a diffuse and/or shock-heated phase that is less capable of condensing into molecular clouds. Of all optical lines, ${rm M_{H, {small I}}/{M_}}$ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between ${rm M_{H, {small I}}/{M_}}$ and gas-phase metallicity. Residuals in the ${rm M_{H, {small I}}/{M_}}$−EW(O) relation are again correlated with [O i]/H α and H α surface brightness, suggesting they are also driven by variations in the fraction of diffuse and/or shock-heated gas. We recover the strong anticorrelation between ${rm M_{H, {small I}}/{M_}}$ and gas-phase metallicity seen in previous studies. We also find a relationship between ${rm M_{H, {small I}}/{M_}}$ and [O i]6302/H α, suggesting that higher fractions of diffuse and/or shock-heated gas are more prevalent in gas-rich galaxies.
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DOI：
10.1086/163294
发表时间：
1985-07
期刊：
The Astrophysical Journal
影响因子：
--
作者：
R. J. Reynolds
通讯作者：
R. J. Reynolds
DOI：
10.1086/505575
发表时间：
2006-05
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
E. Voges;R. Walterbos
通讯作者：
E. Voges;R. Walterbos
DOI：
10.1086/517867
发表时间：
2007-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
M. Oey;G. Meurer;S. Yelda;S. Yelda;E. Furst;S. M. Caballero-Nieves;S. M. Caballero-Nieves;D. Hanish;Emily M. Levesque;D. Thilker;G. Walth;J. Bland-Hawthorn;M. Dopita;H. Ferguson;T. Heckman;M. Doyle;M. Drinkwater;Kenneth C. Freeman;R. Kennicutt;V. Kilborn;V. Kilborn;P. Knezek;Baerbel S. Koribalski;Martin Meyer;M. Putman;E. Ryan-Weber;R. C. Smith;L. Staveley-Smith;Rachel L. Webster;J. Werk;M. Zwaan
通讯作者：
M. Oey;G. Meurer;S. Yelda;S. Yelda;E. Furst;S. M. Caballero-Nieves;S. M. Caballero-Nieves;D. Hanish;Emily M. Levesque;D. Thilker;G. Walth;J. Bland-Hawthorn;M. Dopita;H. Ferguson;T. Heckman;M. Doyle;M. Drinkwater;Kenneth C. Freeman;R. Kennicutt;V. Kilborn;V. Kilborn;P. Knezek;Baerbel S. Koribalski;Martin Meyer;M. Putman;E. Ryan-Weber;R. C. Smith;L. Staveley-Smith;Rachel L. Webster;J. Werk;M. Zwaan
DOI：
10.1016/s0140-6736(01)38320-4
发表时间：
1910-05
期刊：
The Lancet
影响因子：
--
作者：
James Troup;G. Maynard
通讯作者：
James Troup;G. Maynard
DOI：
10.1086/311154
发表时间：
1998-01
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
R. J. Reynolds;N. Hausen;S. Tufte;L. M. Haffner
通讯作者：
R. J. Reynolds;N. Hausen;S. Tufte;L. M. Haffner