The Astrophysical Journal Letters (Jan 2023)
Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
- Vikram Ravi,
- Morgan Catha,
- Ge Chen,
- Liam Connor,
- Jakob T. Faber,
- James W. Lamb,
- Gregg Hallinan,
- Charlie Harnach,
- Greg Hellbourg,
- Rick Hobbs,
- David Hodge,
- Mark Hodges,
- Casey Law,
- Paul Rasmussen,
- Kritti Sharma,
- Myles B. Sherman,
- Jun Shi,
- Dana Simard,
- Reynier Squillace,
- Sander Weinreb,
- David P. Woody,
- Nitika Yadlapalli,
- The Deep Synoptic Array team,
- Tomas Ahumada,
- Dillon Dong,
- Christoffer Fremling,
- Yuping Huang,
- Viraj Karambelkar,
- Jessie M. Miller
Affiliations
- Vikram Ravi
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Morgan Catha
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Ge Chen
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Liam Connor
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Jakob T. Faber
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- James W. Lamb
- ORCiD
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Gregg Hallinan
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Charlie Harnach
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Greg Hellbourg
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Rick Hobbs
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- David Hodge
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Mark Hodges
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Casey Law
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Paul Rasmussen
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Kritti Sharma
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Myles B. Sherman
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Jun Shi
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Dana Simard
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Reynier Squillace
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Sander Weinreb
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- David P. Woody
- Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
- Nitika Yadlapalli
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- The Deep Synoptic Array team
- Tomas Ahumada
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Dillon Dong
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Christoffer Fremling
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Yuping Huang
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Viraj Karambelkar
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- Jessie M. Miller
- ORCiD
- Cahill Center for Astronomy and Astrophysics , MC 249-17 California Institute of Technology, Pasadena, CA 91125, USA ; [email protected]
- DOI
- https://doi.org/10.3847/2041-8213/acc4b6
- Journal volume & issue
-
Vol. 949,
no. 1
p. L3
Abstract
We report the detection and interferometric localization of the repeating fast radio burst (FRB) source FRB 20220912A during commissioning observations with the Deep Synoptic Array (DSA-110). Two bursts were detected from FRB 20220912A, one each on 2022 October 18 and 2022 October 25. The best-fit position is (R.A. J2000, decl. J2000) = (23:09:04.9, +48:42:25.4), with a 90% confidence error ellipse with radii ±2″ and ±1″ in R.A. and decl., respectively. The two bursts are polarized, and we find a Faraday rotation measure that is consistent with the low value of +0.6 rad m ^−2 reported by CHIME/FRB. The DSA-110 localization overlaps with the galaxy PSO J347.2702+48.7066 at a redshift z = 0.0771, which we identify as the likely host. PSO J347.2702+48.7066 has a stellar mass of approximately 10 ^10 M _⊙ , modest internal dust extinction, and a star formation rate likely in excess of 0.1 M _⊙ yr ^−1 . The host-galaxy contribution to the dispersion measure is likely ≲50 pc cm ^−3 . The FRB 20220912A source is therefore likely viewed along a tenuous plasma column through the host galaxy.
Keywords
