2017A&A...608A.138G


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET00:45:41

2017A&A...608A.138G - Astronomy and Astrophysics, volume 608A, 138-138 (2017/12-1)

The ALMA Frontier Fields Survey. III. 1.1 mm emission line identifications in Abell 2744, MACSJ 0416.1-2403, MACSJ 1149.5+2223, Abell 370, and Abell S1063.

GONZALEZ-LOPEZ J., BAUER F.E., ARAVENA M., LAPORTE N., BRADLEY L., CARRASCO M., CARVAJAL R., DEMARCO R., INFANTE L., KNEISSL R., KOEKEMOER A.M., MUNOZ ARANCIBIA A.M., TRONCOSO P., VILLARD E. and ZITRIN A.

Abstract (from CDS):

Context. Most sub-mm emission line studies of galaxies to date have targeted sources with known redshifts where the frequencies of the lines are well constrained. Recent blind line scans circumvent the spectroscopic redshift requirement, which could represent a selection bias.
Aims. Our aim is to detect emission lines present in continuum oriented observations. The detection of these lines provides spectroscopic redshift information and yields important properties of the galaxies.
Methods. We perform a search for emission lines in the Atacama Large Millimeter/submillimeter Array observations of five clusters which are part of the Frontier Fields and assess the reliability of our detection. We additionally investigate plausibility by associating line candidates with detected galaxies in deep near-infrared imaging.
Results. We find 26 significant emission lines candidates, with observed line fluxes between 0.2-4.6Jy.km/s and velocity dispersions (FWHM) of 25-600km/s. Nine of these candidates lie in close proximity to near-infrared sources, boosting their reliability; in six cases the observed line frequency and strength are consistent with expectations given the photometric redshift and properties of the galaxy counterparts. We present redshift identifications, magnifications, and molecular gas estimates for the galaxies with identified lines. We show that two of these candidates likely originate from starburst galaxies, one of which is a so-called jellyfish galaxy that is strongly affected by ram pressure stripping, while another two are consistent with being main sequence galaxies based in their depletion times.
Conclusions. This work highlights the degree to which serendipitous emission lines can be discovered in large mosaic continuum observations when deep ancillary data are available. The low number of high-significance line detections, however, confirms that such surveys are not as optimal as blind line scans. We stress that Monte Carlo simulations should be used to assess the line detection significances since using the negative noise suffers from stochasticity and incurs significantly larger uncertainties.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: high-redshift - gravitational lensing: strong - submillimeter: ISM - ISM: lines and bands - ISM: lines and bands

Nomenclature: Tables 2-3: [GBA2017] A2744-ELNN (Nos 01-03), [GBA2017] MACSJ0416-ELNN (Nos 01-06), [GBA2017] MACSJ1149-ELNN (Nos 01-03), [GBA2017] A370-ELNN (Nos 01-05), [GBA2017] AS1063-ELNN (Nos 01-09).

Simbad objects: 35

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Number of rows : 35

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 [GBA2017] A2744-EL02 EmO 00 14 16.290 -30 24 22.44           ~ 1 0
2 [GBA2017] A2744-EL01 EmO 00 14 18.430 -30 24 47.50           ~ 1 0
3 [GBA2017] A2744-EL03 EmO 00 14 18.880 -30 23 45.60           ~ 1 0
4 ACO 2744 ClG 00 14 20.03 -30 23 17.8           ~ 584 0
5 [GBA2017] A370-EL02 EmO 02 39 50.420 -01 34 40.86           ~ 1 0
6 ACO 370 ClG 02 39 50.5 -01 35 08           ~ 647 0
7 BOW ACO 370 CC128 GiC 02 39 51.020 -01 33 45.39           ~ 8 0
8 [GBA2017] A370-EL03 EmO 02 39 52.460 -01 35 35.33           ~ 1 0
9 [GBA2017] A370-EL04 EmO 02 39 53.250 -01 33 49.13           ~ 1 0
10 [GBA2017] A370-EL05 EmO 02 39 55.260 -01 34 43.13           ~ 1 0
11 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1320 0
12 MCS J0416.1-2403 ClG 04 16 08.380 -24 04 20.80           ~ 225 0
13 [GBA2017] MACSJ0416-EL06 EmO 04 16 08.680 -24 03 42.37           ~ 1 0
14 [GBA2017] MACSJ0416-EL02 EmO 04 16 09.240 -24 05 21.67           ~ 1 0
15 [GBA2017] MACSJ0416-EL01 EmO 04 16 10.170 -24 04 37.82           ~ 1 0
16 [GBA2017] MACSJ0416-EL03 EmO 04 16 10.500 -24 05 05.47           ~ 1 0
17 [GBA2017] MACSJ0416-EL04 EmO 04 16 10.560 -24 04 02.67           ~ 1 0
18 [GBA2017] MACSJ0416-EL05 EmO 04 16 12.320 -24 05 02.47           ~ 1 0
19 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 372 0
20 [GBA2017] MACSJ1149-EL02 EmO 11 49 34.670 +22 23 44.40           ~ 1 0
21 MCS J1149.5+2223 ClG 11 49 35.8 +22 23 55           ~ 335 0
22 [GBA2017] MACSJ1149-EL01 EmO 11 49 36.090 +22 23 47.90           ~ 1 0
23 [GBA2017] MACSJ1149-EL03 EmO 11 49 38.370 +22 24 30.60           ~ 1 0
24 QSO B1202-074 QSO 12 05 23.12 -07 42 32.4     17.5     ~ 352 5
25 NAME Hubble Deep Field reg 12 36 49.5 +62 12 58           ~ 1838 1
26 [ESE2014] RXJ2248-JFG1 G 22 48 40.140 -44 30 50.11     20.66   20.18 ~ 5 0
27 [GBA2017] AS1063-EL04 EmO 22 48 40.370 -44 31 58.00           ~ 1 0
28 [GBA2017] AS1063-EL08 EmO 22 48 42.980 -44 31 55.70           ~ 1 0
29 [GBA2017] AS1063-EL09 EmO 22 48 43.350 -44 32 31.40           ~ 1 0
30 [GBA2017] AS1063-EL05 EmO 22 48 43.650 -44 31 35.60           ~ 1 0
31 [GBA2017] AS1063-EL06 EmO 22 48 47.260 -44 31 49.20           ~ 1 0
32 [GBA2017] AS1063-EL03 EmO 22 48 47.450 -44 32 59.00           ~ 1 0
33 [GBA2017] AS1063-EL02 EmO 22 48 48.030 -44 31 11.55           ~ 1 0
34 [GBA2017] AS1063-EL07 EmO 22 48 48.420 -44 31 50.05           ~ 1 0
35 ACO S 1063 ClG 22 48 54.3 -44 31 07           ~ 214 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-00:45:41

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