HI-MaNGA : tracing the physics of the neutral and ionized ISM with the second data release

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 (MH I/M∗) and average ISM/star formation properties probed by optical emission lines. MH 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 MH 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, MH I/M∗ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between MH I/M∗ and gas-phase metallicity. Residuals in the MH 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 MH I/M∗ and gas-phase metallicity seen in previous studies. We also find a relationship between MH 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

A MultiWavelength Study of the Symbiotic Mira HM Sge with SOFIA and HST

We have targeted the dusty symbiotic mira system HM Sge with four instruments from the IR to the UV. We have used these observations along with archival observations to study how the system has been evolving after its 1975 nova-like outburst. We have detected ro-vibrational water emission in a symbiotic system for the first time using new EXES high spectral resolution infrared spectroscopy. The features, detected in emission, have velocities consistent with the systemic velocity but do not show any clear evidence of high velocity outflows. Mid-infrared photometry and grism spectroscopy show that the oxygen-rich Asymptotic Giant Branch (AGB) dust and dust output has shown little to no change over the past 39 years. In the optical/UV, we detect three main [NII] nebular features that were detected 22 years ago. Two of these features show a small amount of movement corresponding to average outflows speeds of 38 kms and 78 kms since they were previously observed; some previously detected [NII] features are no longer visible. New UV spectroscopy has shown that the nebular environment continues to steadily relax after the system's 1975 outburst. The data suggest however, that the hot component has increased in temperature from 200,000 K in 1989 to now greater than 250,000 K. Our new and archival observations suggest that the evolution of the system after its outburst is swift with little to no major changes after a period of a couple years.Comment: Accepted in Ap

The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

This paper documents the 16th data release (DR16) from the Sloan Digital Sky Surveys (SDSS), the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the Southern Hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey and new data from the SPectroscopic IDentification of ERosita Survey programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17)

The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

This paper documents the 16th data release (DR16) from the Sloan Digital Sky Surveys (SDSS), the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the Southern Hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey and new data from the SPectroscopic IDentification of ERosita Survey programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17)

HI-MaNGA : tracing the physics of the neutral and ionized ISM with the second data release

Funding: VAR acknowledges financial support from CONACyT grant 285721. ZZ acknowledges support by NSFC grant U1931110.Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions.We present the second data release for the HI-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 (⁠MHI/M∗MHI/M∗⁠) and average ISM/star formation properties probed by optical emission lines. MHI/M∗MHI/M∗ is very weakly correlated with the equivalent width of Hα, implying a loose connection between the instantaneous star formation rate and the HI reservoir, although the link between MHI/M∗MHI/M∗ and star formation strengthens when averaged even over only moderate timescales (∼30 Myrs). Galaxies with elevated H I depletion times have enhanced [O I]/Hα and depressed Hα surface brightness, consistent with more H I residing in a diffuse and/or shock heated phase which is less capable of condensing into molecular clouds. Of all optical lines, MHI/M∗MHI/M∗ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between MHI/M∗MHI/M∗ and gas-phase metallicity. Residuals in the MHI/M∗MHI/M∗−EW(O) relation are again correlated with [O I]/Hα and Hα surface brightness, suggesting they are also driven by variations in the fraction of diffuse and/or shock-heated gas. We recover the strong anti-correlation between MHI/M∗MHI/M∗ and gas-phase metallicity seen in previous studies. We also find a relationship between MHI/M∗MHI/M∗ and [O I]6302/Hα, suggesting that higher fractions of diffuse and/or shock-heated gas are more prevalent in gas-rich galaxies.PostprintPeer reviewe

H_I-MaNGA:tracing the physics of the neutral and ionized ISM with the second data release

We present the second data release for the HI-MaNGA programme of HI 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 HI-to-stellar mass ratio (⁠MHI/M∗⁠) and average ISM/star formation properties probed by optical emission lines. MHI/M∗ is very weakly correlated with the equivalent width of H α, implying a loose connection between the instantaneous star formation rate and the HI reservoir, although the link between MHI/M∗ and star formation strengthens when averaged even over only moderate timescales (∼30 Myrs). Galaxies with elevated HI depletion times have enhanced [OI]/Hα and depressed Hα surface brightness, consistent with more HI residing in a diffuse and/or shock heated phase which is less capable of condensing into molecular clouds. Of all optical lines, MHI/M∗ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between MHI/M∗ and gas-phase metallicity. Residuals in the MHI/M∗−EW(O) relation are again correlated with [OI]/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 anti-correlation between MHI/M∗ and gas-phase metallicity seen in previous studies. We also find a relationship between MHI/M∗ and [OI]6302/H α, suggesting that higher fractions of diffuse and/or shock-heated gas are more prevalent in gas-rich galaxies

H <scp>i</scp>-MaNGA: tracing the physics of the neutral and ionized ISM with the second data release

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.</jats:p