564 citations · 2.6k across the 46 of their papers we have counts for
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Galaxy Properties at the Faint End of the HI Mass Function
Kristen B. W. McQuinn, Anjana K. Telidevara, Jackson Fuson +9
The Survey of HI in Extremely Low-mass Dwarfs (SHIELD) includes a volumetrically complete sample of 82 gas-rich dwarfs with M_HI~<10^7.2 Msun selected from the ALFALFA survey. We a…
The Extragalactic Distance Database: The Color-Magnitude Diagrams and Tip of the Red Giant Branch Distances Catalog
Gagandeep S. Anand, Luca Rizzi, R. Brent Tully +7
The Extragalactic Distance Database (EDD) was created as a repository for high quality, redshift-independent distances. A key component of EDD is the Color Magnitude Diagrams/Tip o…
A Tip of the Red Giant Branch Distance of Mpc to the Dark Matter Deficient Galaxy NGC1052-DF2 from 40 Orbits of Hubble Space Telescope Imaging
Zili Shen, Shany Danieli, Pieter van Dokkum +7
The large and diffuse galaxies NGC1052-DF2 and NGC1052-DF4 have been found to have very low dark matter content and a population of luminous globular clusters. Accurate distance me…
The Masses of Supernova Remnant Progenitors in NGC 6946
Brad Koplitz, Jared Johnson, Benjamin F. Williams +5
We constrained the progenitor masses for 169 supernova remnants, 8 historically observed supernovae, and the black hole formation candidate in NGC 6946, finding that they are consi…
The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) I. Ultraviolet to Infrared Photometry of 22 Million Stars in M33
Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton +18
We present panchromatic resolved stellar photometry for 22 million stars in the Local Group dwarf spiral Triangulum (M33), derived from Hubble Space Telescope (HST) observations wi…
Progenitor Mass Distribution for 22 Historic Core-Collapse Supernovae
Mariangelly Díaz-Rodríguez, Jeremiah W. Murphy, Benjamin F. Williams +2
We infer the progenitor mass distribution for 22 historic core-collapse supernovae (CCSNe) using a Bayesian hierarchical model. For this inference, we use the local star formation…