Where do stars explode in the ISM? -- The distribution of dense gas around evolved massive stars in M33
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| Format: | Preprint |
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2023
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| author | Sarbadhicary, Sumit K. Wagner, Jordan Koch, Eric W. Chen, Ness Mayker Leroy, Adam K. Lahén, Natalia Rosolowsky, Erik Neugent, Kathryn F. Kim, Chang-Goo Chomiuk, Laura Dalcanton, Julianne J. Lopez, Laura A. Pingel, Nickolas M. Indebetouw, Remy Williams, Thomas G. Tarantino, Elizabeth Meyer, Jennifer Donovan Skillman, Evan D. Smercina, Adam Kepley, Amanda A. Murphy, Eric J. Strader, Jay Wong, Tony Stanimirović, Snežana Villanueva, Vicente Walter, Fabian Ott, Juergen Darling, Jeremy Roman-Duval, Julia Murray, Claire E. |
| author_facet | Sarbadhicary, Sumit K. Wagner, Jordan Koch, Eric W. Chen, Ness Mayker Leroy, Adam K. Lahén, Natalia Rosolowsky, Erik Neugent, Kathryn F. Kim, Chang-Goo Chomiuk, Laura Dalcanton, Julianne J. Lopez, Laura A. Pingel, Nickolas M. Indebetouw, Remy Williams, Thomas G. Tarantino, Elizabeth Meyer, Jennifer Donovan Skillman, Evan D. Smercina, Adam Kepley, Amanda A. Murphy, Eric J. Strader, Jay Wong, Tony Stanimirović, Snežana Villanueva, Vicente Walter, Fabian Ott, Juergen Darling, Jeremy Roman-Duval, Julia Murray, Claire E. |
| contents | The effect of supernovae (SNe) on star-formation in the interstellar medium (ISM) depends sensitively on where SNe explode with respect to ISM clouds. Observationally, SN ISM environments characterized by spatially-resolved gas maps can empirically guide the placement of SNe in subgrid models, but unfortunately such measurements remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach -- mapping the ISM around evolved massive stars that are soon to explode. These provide a substantially larger sample of `explosion sites' (than just historical SNe) in nearby galaxies that have high-resolution atomic and molecular ISM maps from Jansky VLA and ALMA. We demonstrate this technique in the well-resolved Local Group spiral M33 by analyzing the 50 pc-scale projected ISM densities around red supergiants (RSGs, 8-30 M$_{\odot}$ stars) Wolf-Rayet stars (WRs, $>$30 M$_{\odot}$ stars), and supernova remnants (SNRs). We find a \emph{mass-dependent} correlation between stars and gas clouds, with atleast 45\% of WRs and upto 77\% of RSGs having no detectable H$_2$ at their pixel locations. In the sample with H$_2$ detections, we find that more massive younger progenitors are coincident with denser gas. We show that the density distributions for stars $>$15 M$_{\odot}$ are statistically distinct from random alignment of stars and gas in M33. Our work provides the first observationally-derived estimate of the fraction of the SN-producing stellar population correlated with ISM density peaks. We demonstrate how this can be compared with galaxy simulations, and advocate similar comparisons to the community for constraining sub-grid models. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_17694 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Where do stars explode in the ISM? -- The distribution of dense gas around evolved massive stars in M33 Sarbadhicary, Sumit K. Wagner, Jordan Koch, Eric W. Chen, Ness Mayker Leroy, Adam K. Lahén, Natalia Rosolowsky, Erik Neugent, Kathryn F. Kim, Chang-Goo Chomiuk, Laura Dalcanton, Julianne J. Lopez, Laura A. Pingel, Nickolas M. Indebetouw, Remy Williams, Thomas G. Tarantino, Elizabeth Meyer, Jennifer Donovan Skillman, Evan D. Smercina, Adam Kepley, Amanda A. Murphy, Eric J. Strader, Jay Wong, Tony Stanimirović, Snežana Villanueva, Vicente Walter, Fabian Ott, Juergen Darling, Jeremy Roman-Duval, Julia Murray, Claire E. Astrophysics of Galaxies The effect of supernovae (SNe) on star-formation in the interstellar medium (ISM) depends sensitively on where SNe explode with respect to ISM clouds. Observationally, SN ISM environments characterized by spatially-resolved gas maps can empirically guide the placement of SNe in subgrid models, but unfortunately such measurements remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach -- mapping the ISM around evolved massive stars that are soon to explode. These provide a substantially larger sample of `explosion sites' (than just historical SNe) in nearby galaxies that have high-resolution atomic and molecular ISM maps from Jansky VLA and ALMA. We demonstrate this technique in the well-resolved Local Group spiral M33 by analyzing the 50 pc-scale projected ISM densities around red supergiants (RSGs, 8-30 M$_{\odot}$ stars) Wolf-Rayet stars (WRs, $>$30 M$_{\odot}$ stars), and supernova remnants (SNRs). We find a \emph{mass-dependent} correlation between stars and gas clouds, with atleast 45\% of WRs and upto 77\% of RSGs having no detectable H$_2$ at their pixel locations. In the sample with H$_2$ detections, we find that more massive younger progenitors are coincident with denser gas. We show that the density distributions for stars $>$15 M$_{\odot}$ are statistically distinct from random alignment of stars and gas in M33. Our work provides the first observationally-derived estimate of the fraction of the SN-producing stellar population correlated with ISM density peaks. We demonstrate how this can be compared with galaxy simulations, and advocate similar comparisons to the community for constraining sub-grid models. |
| title | Where do stars explode in the ISM? -- The distribution of dense gas around evolved massive stars in M33 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2310.17694 |