Physical Characterization of Serendipitously Uncovered Millimeter-wave Line-emitting Galaxies at z∼2.5 behind the Local Luminous Infrared Galaxy VV 114 Mizukoshi, Shoichiro Espada Fernández, Daniel We thank the anonymous referee for a number of insightful comments and suggestions that greatly improved the quality of this paper. Data analysis was partly carried out on the common-use data analysis computer system at the Astronomy Data Center (ADC) of the National Astronomical Observatory of Japan (NAOJ). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.01057.S, #2015.1.00973.S, #2015.1.00902.S, and #2013.1.00740.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work was supported by JSPS KAKENHI grant No. JP17H06130 and by the NAOJ ALMA Scientific Research grant No. 2017-06B. F.E. is supported by JSPS KAKENHI grant No. 17K14259. D.E. acknowledges support from a Beatriz Galindo senior fellowship (BG20/00224) from the Spanish Ministry of Science and Innovation. D. I. is supported by JSPS KAKENHI grant No. 321H01133. We present a detailed investigation of millimeter-wave line emitters ALMA J010748.3-173028 (ALMA-J0107a) and ALMA J010747.0-173010 (ALMA-J0107b), which were serendipitously uncovered in the background of the nearby galaxy VV 114 with spectral scan observations at lambda = 2-3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA) detection of CO(4-3), CO(3-2), and [C i](1-0) lines for both sources, their spectroscopic redshifts are unambiguously determined to be z = 2.4666 +/- 0.0002 and z = 2.3100 +/- 0.0002, respectively. We obtain the apparent molecular gas masses M-gas of these two line emitters from [C i] line fluxes as (11.2 +/- 3.1) x 10(10) M-circle dot and (4.2 +/- 1.2) x 10(10) M-circle dot, respectively. The observed CO(4-3) velocity field of ALMA-J0107a exhibits a clear velocity gradient across the CO disk, and we find that ALMA-J0107a is characterized by an inclined rotating disk with a significant turbulence, that is, a deprojected maximum rotation velocity to velocity dispersion ratio v(max)/sigma(v) of 1.3 +/- 0.3. We find that the dynamical mass of ALMA-J0107a within the CO-emitting disk computed from the derived kinetic parameters, (1.1 +/- 0.2) x 10(10) M-circle dot, is an order of magnitude smaller than the molecular gas mass derived from dust continuum emission, (3.2 +/- 1.6) x 10(11) M-circle dot. We suggest this source is magnified by a gravitational lens with a magnification of mu greater than or similar to 10, which is consistent with the measured offset from the empirical correlation between CO-line luminosity and width. 2021-11-12T09:52:40Z 2021-11-12T09:52:40Z 2021-05-20 journal article Published version: Shoichiro Mizukoshi... [et al.] 2021 ApJ 917 94. [https://doi.org/10.3847/1538-4357/ac01cc] http://hdl.handle.net/10481/71465 eng http://creativecommons.org/licenses/by/3.0/es/ open access Atribución 3.0 España Institute of Physics Publishing