Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2503.20042 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866915213661437952 |
|---|---|
| author | Ha, Triet Rupke, David Caraker, Shane Harper, Jack Coil, Alison Li, Miao Tremonti, Christy Diamond-Stanic, Aleksandar Geach, James Hickox, Ryan Johnson, Sean Leung, Gene Moustakas, John Perrotta, Serena Rudnick, Gregory Sell, Paul Whalen, Kelly |
| author_facet | Ha, Triet Rupke, David Caraker, Shane Harper, Jack Coil, Alison Li, Miao Tremonti, Christy Diamond-Stanic, Aleksandar Geach, James Hickox, Ryan Johnson, Sean Leung, Gene Moustakas, John Perrotta, Serena Rudnick, Gregory Sell, Paul Whalen, Kelly |
| contents | The OVI 1032, 1038 A line is a key probe of cooling gas in the circumgalactic medium (CGM) of galaxies, but has been observed to date primarily in absorption along single sightlines. We present deep HST ACS-SBC observations of the compact, massive starburst Makani. Makani hosts a 100 kpc, [OII]-emitting galactic wind driven by two episodes of star formation over 400 Myr. We detect OVI and Ly$α$ emission across the [OII] nebula with similar morphology and extent, out to r ~ 50 kpc. Using differential narrow-band imaging, we separate Ly$α$ and OVI and show that the OVI emission is comparable in brightness to [OII], with $L_{OVI} = 4\times10^{42}$ erg/s. The similar hourglass morphology and size of [OII] and OVI implicate radiative cooling at $T = 10^{5.5}$ K in a hot-cold interface. This may occur as the $T > 10^7$ K CGM -- or the hot fluid driving the wind -- exchanges mass with the $T \approx 10^4$ K clouds entrained in (or formed by) the wind. The optical/UV line ratios may be consistent with shock ionization, though uncertain attenuation and Ly$α$ radiative transfer complicate the interpretation. The detection of OVI in Makani lies at the bleeding edge of the UV imaging capabilities of HST, and provides a benchmark for future emission-line imaging of the CGM with a wide-area UV telescope. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_20042 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Deep Ultraviolet, Emission-Line Imaging of the Makani Galactic Wind Ha, Triet Rupke, David Caraker, Shane Harper, Jack Coil, Alison Li, Miao Tremonti, Christy Diamond-Stanic, Aleksandar Geach, James Hickox, Ryan Johnson, Sean Leung, Gene Moustakas, John Perrotta, Serena Rudnick, Gregory Sell, Paul Whalen, Kelly Astrophysics of Galaxies The OVI 1032, 1038 A line is a key probe of cooling gas in the circumgalactic medium (CGM) of galaxies, but has been observed to date primarily in absorption along single sightlines. We present deep HST ACS-SBC observations of the compact, massive starburst Makani. Makani hosts a 100 kpc, [OII]-emitting galactic wind driven by two episodes of star formation over 400 Myr. We detect OVI and Ly$α$ emission across the [OII] nebula with similar morphology and extent, out to r ~ 50 kpc. Using differential narrow-band imaging, we separate Ly$α$ and OVI and show that the OVI emission is comparable in brightness to [OII], with $L_{OVI} = 4\times10^{42}$ erg/s. The similar hourglass morphology and size of [OII] and OVI implicate radiative cooling at $T = 10^{5.5}$ K in a hot-cold interface. This may occur as the $T > 10^7$ K CGM -- or the hot fluid driving the wind -- exchanges mass with the $T \approx 10^4$ K clouds entrained in (or formed by) the wind. The optical/UV line ratios may be consistent with shock ionization, though uncertain attenuation and Ly$α$ radiative transfer complicate the interpretation. The detection of OVI in Makani lies at the bleeding edge of the UV imaging capabilities of HST, and provides a benchmark for future emission-line imaging of the CGM with a wide-area UV telescope. |
| title | Deep Ultraviolet, Emission-Line Imaging of the Makani Galactic Wind |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.20042 |