Hostname: page-component-cd9895bd7-q99xh Total loading time: 0 Render date: 2024-12-25T17:25:32.067Z Has data issue: false hasContentIssue false
  • English
  • Français

The Progressive Integral Step Method (PrISM) for Wide Field 3D Spectral Imaging of Nearby Galaxies: an Overview of the TYPHOON Survey

Published online by Cambridge University Press:  09 June 2023

Kathryn Grasha Open the ORCID record for Kathryn Grasha [Opens in a new window]
Kathryn Grasha*
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia; email: [email protected] ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The TYPHOON program is producing an atlas of spectroscopic data cubes of 44 large-angular-sized galaxies with complete spatial coverage from 3650–9000 Å. This survey provides an unparalleled opportunity to study variations in the interstellar medium (ISM) properties within individual H ii regions across the entire star-forming disks of nearby galaxies. This can provide key insights into the spatial distribution and resolved properties of the ISM to understand how efficiently metals are mixed and redistributed across spirals and dwarf galaxies. In this Proceeding, we present early science results from six nearby spiral galaxies as part of the TYPHOON program from Grasha et al. (2022). We use HIIPhot to identify the H ii regions within the galaxy based on the surface brightness of the Hα emisison line and measure variations of the H ii region oxygen abundance. In this initial work, we find that while the spiral pattern plays a role in organizing the ISM, it alone does not establish the relatively uniform azimuthal variations we observe across all the galaxies. Differences in the metal abundances are more likely driven by the strong correlations with the local physical conditions. We find a strong and positive correlation between the ionization parameter and the local abundances as measured by the relative metallicity offset Δ(O/H), indicating a tight relationship between local physical conditions and their localized enrichment of the ISM. These variations can be explained by a combination of localized, star formation-driven self-enrichment and large-scale mixing-driven dilution due to the passing of spiral density waves.

Keywords

galaxies: abundancesgalaxies: ISMgalaxies: spiralH ii regionsISM: abundancesISM: evolution
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 234 - 241
Check for updates
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Azimlu, M., et al. 2011, AJ, 142, 139 10.1088/0004-6256/142/4/139CrossRefGoogle Scholar
Boissier, S., et al. 1999, MNRAS, 307, 857 10.1046/j.1365-8711.1999.02699.xCrossRefGoogle Scholar
Buder, S., et al. 2022, MNRAS, 510, 2407 Google Scholar
Bundy, K., et al. 2015, ApJ, 798, 7 Google Scholar
Croom, S. M., et al. 2012, MNRAS, noGoogle Scholar
D’Agostino, J. J., et al. 2018, MNRAS, 479, 4907 Google Scholar
Emsellem, E., et al. 2022, A&A, 659, A191 Google Scholar
Grasha, K., et al. 2017, ApJ, 840, 113 10.3847/1538-4357/aa6f15CrossRefGoogle Scholar
Grasha, K., et al. 2018, MNRAS, 481, 1016 10.1093/mnras/sty2154CrossRefGoogle Scholar
Grasha, K., et al. 2022, ApJ, 929, 118 10.3847/1538-4357/ac5ab2CrossRefGoogle Scholar
Ho, I.-T., et al. 2016, Astrophys Space Sci, 361, 280 10.1007/s10509-016-2865-2CrossRefGoogle Scholar
Ho, I.-T., et al.. 2017, ApJ, 846, 39 10.3847/1538-4357/aa8460CrossRefGoogle Scholar
Ho, I.-T., et al. 2018, A&A, 618, A64 10.1051/0004-6361/201833262CrossRefGoogle Scholar
Hopkins, P. F., et al. 2013, MNRAS, 432, 2647 10.1093/mnras/stt723CrossRefGoogle Scholar
Kawamura, A., et al. 2009, ApJS, 184, 1 10.1088/0067-0049/184/1/1CrossRefGoogle Scholar
Kennicutt, R. C. J., et al. 1996, ApJ, 456, 504 10.1086/176675CrossRefGoogle Scholar
Kobayashi, C., et al. 2007, MNRAS, 376, 1465 10.1111/j.1365-2966.2007.11555.xCrossRefGoogle Scholar
Krumholz, M. R., et al. 2019, ARAA, 57, 227 10.1146/annurev-astro-091918-104430CrossRefGoogle Scholar
Poetrodjojo, H., et al. 2019, MNRAS, 487, 79 10.1093/mnras/stz1241CrossRefGoogle Scholar
Rosales-Ortega, F. F., et al. 2010, MNRASGoogle Scholar
Rousseau-Nepton, L., et al. 2019, MNRAS, 489, 5530 Google Scholar
Ryon, J. E., et al. 2017, ApJ, 841, 92 10.3847/1538-4357/aa719eCrossRefGoogle Scholar
Sánchez, S. F., et al. 2012, A&A, 538, A8 Google Scholar
Sun, J., et al. 2020, ApJ, 892, 148 Google Scholar
Sun, J., et al. 2022, AJ, 164, 43 Google Scholar
Thilker, D. A., et al. 2000, AJ, 120, 3070 10.1086/316852CrossRefGoogle Scholar
Torrey, P., et al. 2019, MNRAS, 484, 5587 Google Scholar
de Zeeuw, T. P., et al. 2002, MNRAS, 329, 513 10.1046/j.1365-8711.2002.05059.xCrossRefGoogle Scholar