@article{mizukoshi_physical_2021,
	title = {Physical {Characterization} of {Serendipitously} {Uncovered} {Millimeter}-wave {Line}-emitting {Galaxies} at z{\textasciitilde}2.5 behind the {Local} {Luminous} {Infrared} {Galaxy} {VV114}},
	volume = {2105},
	url = {http://adsabs.harvard.edu/abs/2021arXiv210508894M},
	abstract = {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 VV114 with spectral scan observations at \${\textbackslash}lambda\$ = 2
- 3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA)
detection of CO(4-3), CO(3-2), and [CI](1-0) lines for both sources,
their spectroscopic redshifts are unambiguously determined to be \$z=
2.4666{\textbackslash}pm0.0002\$ and \$z=2.3100{\textbackslash}pm0.0002\$, respectively. We obtain the
apparent molecular gas masses \$M\_\{{\textbackslash}rm gas\}\$ of these two line emitters
from [CI] line fluxes as \$(11.2 {\textbackslash}pm 3.1) {\textbackslash}times 10{\textasciicircum}\{10\} M\_{\textbackslash}odot\$ and
\$(4.2 {\textbackslash}pm 1.2) {\textbackslash}times 10{\textasciicircum}\{10\} M\_{\textbackslash}odot\$, 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\_\{{\textbackslash}rm max\}/{\textbackslash}sigma\_\{v\}\$ of \$1.3 {\textbackslash}pm 0.3\$. We find that the dynamical
mass of ALMA-J0107a within the CO-emitting disk computed from the
derived kinetic parameters, \$(1.1 {\textbackslash}pm 0.2) {\textbackslash}times 10{\textasciicircum}\{10\}{\textbackslash} M\_{\textbackslash}odot\$, is
an order of magnitude smaller than the molecular gas mass derived from
dust continuum emission, \$(3.2{\textbackslash}pm1.6){\textbackslash}times10{\textasciicircum}\{11\}{\textbackslash} M\_\{{\textbackslash}odot\}\$. We
suggest this source is magnified by a gravitational lens with a
magnification of \${\textbackslash}mu {\textbackslash}gtrsim10\$, which is consistent with the measured
offset from the empirical correlation between CO-line luminosity and
width.},
	urldate = {2021-06-04},
	journal = {arXiv e-prints},
	author = {Mizukoshi, S. and Kohno, K. and Egusa, F. and Hatsukade, B. and Minezaki, T. and Saito, T. and Tamura, Y. and Iono, D. and Ueda, J. and Matsuda, Y. and Kawabe, R. and Lee, M. M. and Yun, M. S. and Espada, D.},
	month = may,
	year = {2021},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2105.08894},
}

{"_id":"GnJsFFgaAm3j5LCRs","bibbaseid":"mizukoshi-kohno-egusa-hatsukade-minezaki-saito-tamura-iono-etal-physicalcharacterizationofserendipitouslyuncoveredmillimeterwavelineemittinggalaxiesatztextasciitilde25behindthelocalluminousinfraredgalaxyvv114-2021","author_short":["Mizukoshi, S.","Kohno, K.","Egusa, F.","Hatsukade, B.","Minezaki, T.","Saito, T.","Tamura, Y.","Iono, D.","Ueda, J.","Matsuda, Y.","Kawabe, R.","Lee, M. M.","Yun, M. S.","Espada, D."],"bibdata":{"bibtype":"article","type":"article","title":"Physical Characterization of Serendipitously Uncovered Millimeter-wave Line-emitting Galaxies at z\\textasciitilde2.5 behind the Local Luminous Infrared Galaxy VV114","volume":"2105","url":"http://adsabs.harvard.edu/abs/2021arXiv210508894M","abstract":"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 VV114 with spectral scan observations at \\${\\textbackslash}lambda\\$ = 2 - 3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA) detection of CO(4-3), CO(3-2), and [CI](1-0) lines for both sources, their spectroscopic redshifts are unambiguously determined to be \\$z= 2.4666{\\textbackslash}pm0.0002\\$ and \\$z=2.3100{\\textbackslash}pm0.0002\\$, respectively. We obtain the apparent molecular gas masses \\$M_\\{{\\textbackslash}rm gas\\}\\$ of these two line emitters from [CI] line fluxes as \\$(11.2 {\\textbackslash}pm 3.1) {\\textbackslash}times 10{\\textasciicircum}\\{10\\} M_{\\textbackslash}odot\\$ and \\$(4.2 {\\textbackslash}pm 1.2) {\\textbackslash}times 10{\\textasciicircum}\\{10\\} M_{\\textbackslash}odot\\$, 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_\\{{\\textbackslash}rm max\\}/{\\textbackslash}sigma_\\{v\\}\\$ of \\$1.3 {\\textbackslash}pm 0.3\\$. We find that the dynamical mass of ALMA-J0107a within the CO-emitting disk computed from the derived kinetic parameters, \\$(1.1 {\\textbackslash}pm 0.2) {\\textbackslash}times 10{\\textasciicircum}\\{10\\}{\\textbackslash} M_{\\textbackslash}odot\\$, is an order of magnitude smaller than the molecular gas mass derived from dust continuum emission, \\$(3.2{\\textbackslash}pm1.6){\\textbackslash}times10{\\textasciicircum}\\{11\\}{\\textbackslash} M_\\{{\\textbackslash}odot\\}\\$. We suggest this source is magnified by a gravitational lens with a magnification of \\${\\textbackslash}mu {\\textbackslash}gtrsim10\\$, which is consistent with the measured offset from the empirical correlation between CO-line luminosity and width.","urldate":"2021-06-04","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Mizukoshi"],"firstnames":["S."],"suffixes":[]},{"propositions":[],"lastnames":["Kohno"],"firstnames":["K."],"suffixes":[]},{"propositions":[],"lastnames":["Egusa"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Hatsukade"],"firstnames":["B."],"suffixes":[]},{"propositions":[],"lastnames":["Minezaki"],"firstnames":["T."],"suffixes":[]},{"propositions":[],"lastnames":["Saito"],"firstnames":["T."],"suffixes":[]},{"propositions":[],"lastnames":["Tamura"],"firstnames":["Y."],"suffixes":[]},{"propositions":[],"lastnames":["Iono"],"firstnames":["D."],"suffixes":[]},{"propositions":[],"lastnames":["Ueda"],"firstnames":["J."],"suffixes":[]},{"propositions":[],"lastnames":["Matsuda"],"firstnames":["Y."],"suffixes":[]},{"propositions":[],"lastnames":["Kawabe"],"firstnames":["R."],"suffixes":[]},{"propositions":[],"lastnames":["Lee"],"firstnames":["M.","M."],"suffixes":[]},{"propositions":[],"lastnames":["Yun"],"firstnames":["M.","S."],"suffixes":[]},{"propositions":[],"lastnames":["Espada"],"firstnames":["D."],"suffixes":[]}],"month":"May","year":"2021","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2105.08894","bibtex":"@article{mizukoshi_physical_2021,\n\ttitle = {Physical {Characterization} of {Serendipitously} {Uncovered} {Millimeter}-wave {Line}-emitting {Galaxies} at z{\\textasciitilde}2.5 behind the {Local} {Luminous} {Infrared} {Galaxy} {VV114}},\n\tvolume = {2105},\n\turl = {http://adsabs.harvard.edu/abs/2021arXiv210508894M},\n\tabstract = {We present a detailed investigation of millimeter-wave line emitters \nALMA J010748.3-173028 (ALMA-J0107a) and ALMA J010747.0-173010\n(ALMA-J0107b), which were serendipitously uncovered in the background of\nthe nearby galaxy VV114 with spectral scan observations at \\${\\textbackslash}lambda\\$ = 2\n- 3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA)\ndetection of CO(4-3), CO(3-2), and [CI](1-0) lines for both sources,\ntheir spectroscopic redshifts are unambiguously determined to be \\$z=\n2.4666{\\textbackslash}pm0.0002\\$ and \\$z=2.3100{\\textbackslash}pm0.0002\\$, respectively. We obtain the\napparent molecular gas masses \\$M\\_\\{{\\textbackslash}rm gas\\}\\$ of these two line emitters\nfrom [CI] line fluxes as \\$(11.2 {\\textbackslash}pm 3.1) {\\textbackslash}times 10{\\textasciicircum}\\{10\\} M\\_{\\textbackslash}odot\\$ and\n\\$(4.2 {\\textbackslash}pm 1.2) {\\textbackslash}times 10{\\textasciicircum}\\{10\\} M\\_{\\textbackslash}odot\\$, respectively. The observed\nCO(4-3) velocity field of ALMA-J0107a exhibits a clear velocity gradient\nacross the CO disk, and we find that ALMA-J0107a is characterized by an\ninclined rotating disk with a significant turbulence, that is, a\ndeprojected maximum rotation velocity to velocity dispersion ratio\n\\$v\\_\\{{\\textbackslash}rm max\\}/{\\textbackslash}sigma\\_\\{v\\}\\$ of \\$1.3 {\\textbackslash}pm 0.3\\$. We find that the dynamical\nmass of ALMA-J0107a within the CO-emitting disk computed from the\nderived kinetic parameters, \\$(1.1 {\\textbackslash}pm 0.2) {\\textbackslash}times 10{\\textasciicircum}\\{10\\}{\\textbackslash} M\\_{\\textbackslash}odot\\$, is\nan order of magnitude smaller than the molecular gas mass derived from\ndust continuum emission, \\$(3.2{\\textbackslash}pm1.6){\\textbackslash}times10{\\textasciicircum}\\{11\\}{\\textbackslash} M\\_\\{{\\textbackslash}odot\\}\\$. We\nsuggest this source is magnified by a gravitational lens with a\nmagnification of \\${\\textbackslash}mu {\\textbackslash}gtrsim10\\$, which is consistent with the measured\noffset from the empirical correlation between CO-line luminosity and\nwidth.},\n\turldate = {2021-06-04},\n\tjournal = {arXiv e-prints},\n\tauthor = {Mizukoshi, S. and Kohno, K. and Egusa, F. and Hatsukade, B. and Minezaki, T. and Saito, T. and Tamura, Y. and Iono, D. and Ueda, J. and Matsuda, Y. and Kawabe, R. and Lee, M. M. and Yun, M. S. and Espada, D.},\n\tmonth = may,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2105.08894},\n}\n\n","author_short":["Mizukoshi, S.","Kohno, K.","Egusa, F.","Hatsukade, B.","Minezaki, T.","Saito, T.","Tamura, Y.","Iono, D.","Ueda, J.","Matsuda, Y.","Kawabe, R.","Lee, M. M.","Yun, M. S.","Espada, D."],"key":"mizukoshi_physical_2021","id":"mizukoshi_physical_2021","bibbaseid":"mizukoshi-kohno-egusa-hatsukade-minezaki-saito-tamura-iono-etal-physicalcharacterizationofserendipitouslyuncoveredmillimeterwavelineemittinggalaxiesatztextasciitilde25behindthelocalluminousinfraredgalaxyvv114-2021","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2021arXiv210508894M"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["physical","characterization","serendipitously","uncovered","millimeter","wave","line","emitting","galaxies","textasciitilde2","behind","local","luminous","infrared","galaxy","vv114","mizukoshi","kohno","egusa","hatsukade","minezaki","saito","tamura","iono","ueda","matsuda","kawabe","lee","yun","espada"],"title":"Physical Characterization of Serendipitously Uncovered Millimeter-wave Line-emitting Galaxies at z\\textasciitilde2.5 behind the Local Luminous Infrared Galaxy VV114","year":2021}