Summary - The Evolution of Gas in and around Galaxies. Online registration by Cvent

The evolution of the hydrogen content of galaxies and their surroundings dictates the evolution of the star formation activity of the Universe. Observationally, it is now well established that the star formation activity of the Universe evolves over time, with a broad peak at redshifts ~ 1-3, and then a decline by an order of magnitude to z=0. However, we know very little about the evolution of the fuel for this star formation, the neutral gas content of galaxies, over this period.

Recently, several telescopes have become operational that can detect HI 21cm emission out to redshifts of 1 and beyond (e.g. the GMRT, MeerKAT, ASKAP, and JVLA). Deep HI 21cm observations of nearby galaxies with these and other facilities have begun to probe diffuse HI in the circumgalactic medium (CGM), while HI 21cm mapping studies have yielded exquisite rotation curves, providing detailed information on galaxy kinematics. It is now possible to study not only the evolution of the HI content of galaxies, but also scaling relations with other galaxy properties, morphology with respect to the galaxy's location in the cosmic web, gas accretion, and the role of HI in galaxy evolution. At high redshifts, C+ mapping studies have yielded rotation curves of early galaxies, complementing the HI 21cm mapping studies in the nearby Universe. And, absorption studies have yielded a wealth of information on gas in the CGM and its redshift evolution.

The goal of this meeting is to compare and contrast the results of these different HI 21cm, C+, and CGM observations, to compare them to theoretical predictions, and to place the new results in the context of galaxy evolution. The meeting is extremely timely as the first results of the different HI 21cm surveys are just beginning to appear.

The meeting will examine our understanding of the evolution of hydrogen in and around galaxies, by addressing the following questions:

1. How does the HI content, morphology, and kinematics of galaxies evolve with redshift?

2. How does the HI content of a galaxy relate to other galaxy properties (e.g., environment, SFR, stellar content, CGM properties, etc)?

3. How does the gas accretion rate evolve with redshift? Is the SFR limited by the neutral hydrogen reservoir or the gas accretion rate, or both?

4. How well do numerical simulations reproduce the gas properties, and redshift evolution, of galaxies and their CGM, and what does this tell us about the role of HI in galaxy evolution?

5. How does the gas move from the CGM of galaxies to their disks, and transition from the ionized to the neutral phase, at different redshifts?

6. What can observations of high-z galaxies learn from the wealth of detailed studies at z~0?

November 6, 2022: Submissions for Expressions of Interest open
December 15, 2022: First Review of Expressions of Interest
Mid-to late December: First Round of Invitations to Attend sent out
January 31, 2023: Submission for Expressions of Interest close
Early February: Remainder of Invitations to Attend sent out
March 3, 2023: Abstract and Travel Support Application deadline
April 10, 2023: Announcement of Science Program and Travel Support Recipients
April 10, 2023: Registration and Housing Requests open
May 1, 2023: Registration and Housing Requests close
May 22, 2023: Payment Invoices distributed
June 16, 2023: Registration Fee and Accommodations Payment deadline
July 1, 2023: Airport Shuttle Registration deadline
July 31 to August 4, 2023: Meeting in Stanley, ID