2012AJ....144..123O

Query : 2012AJ....144..123O

2012AJ....144..123O - Astron. J., 144, 123 (2012/October-0)

VLA-ANGST: a high-resolution H I survey of nearby dwarf galaxies.

OTT J., STILP A.M., WARREN S.R., SKILLMAN E.D., DALCANTON J.J., WALTER F., DE BLOK W.J.G., KORIBALSKI B. and WEST A.A.

Abstract (from CDS):

We present the "Very Large Array survey of Advanced Camera for Surveys Nearby Galaxy Survey Treasury galaxies (VLA-ANGST)." VLA-ANGST is a National Radio Astronomy Observatory Large Program consisting of high spectral (0.6-2.6 km/s) and spatial (∼6'') resolution observations of neutral, atomic hydrogen (H I) emission toward 35 nearby dwarf galaxies from the ANGST survey. ANGST is a systematic Hubble Space Telescope survey to establish a legacy of uniform multi-color photometry of resolved stars for a volume-limited sample of nearby galaxies (D ≲ 4 Mpc). VLA-ANGST provides VLA H I observations of the sub-sample of ANGST galaxies with recent star formation that are observable from the northern hemisphere and that were not observed in the "The H I Nearby Galaxy Survey" (THINGS). The overarching scientific goal of VLA-ANGST is to investigate fundamental characteristics of the neutral interstellar medium (ISM) of dwarf galaxies. Here we describe the VLA observations, the data reduction, and the final VLA-ANGST data products. We present an atlas of the integrated H I maps, the intensity-weighted velocity fields, the second moment maps as a measure for the velocity dispersion of the H I, individual channel maps, and integrated H I spectra for each VLA-ANGST galaxy. We closely follow the observational setup and data reduction of THINGS to achieve comparable sensitivity and angular resolution. A major difference between VLA-ANGST and THINGS, however, is the high velocity resolution of the VLA-ANGST observations (0.65 and 1.3 km/s for the majority of the galaxies). The VLA-ANGST data products are made publicly available through a dedicated Web site (https://science.nrao.edu/science/surveys/vla-angst). With available star formation histories from resolved stellar populations and lower resolution ancillary observations from the far-infrared to the ultraviolet, VLA-ANGST will enable detailed studies of the relationship between the ISM and star formation in dwarf galaxies on a ∼100 pc scale.

Abstract Copyright: ∼

Journal keyword(s): galaxies: irregular - galaxies: ISM - galaxies: structure - ISM: atoms - radio lines: galaxies - surveys

CDS comments: Notes Table 4: AO 0952+62 is a misprint for AO 0952+69.

Simbad objects: 43

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Number of rows : 43
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NGC 247 LSB 00 47 08.554 -20 45 37.44 10.11 9.61 9.10 8.87   ~ 441 2
2 NVSS J004713-205114 Rad 00 47 13.5 -20 51 17           ~ 2 0
3 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3344 2
4 ESO 540-31 G 00 49 49.3 -21 00 58 16.11 15.64 15.36 14.8 15.5 ~ 133 1
5 NAME Scl Group GrG 01 00 06 -33 44.2           ~ 509 0
6 NGC 404 LIN 01 09 27.02 +35 43 05.3   12.56 11.73     ~ 478 0
7 3C 48 QSO 01 37 41.2996631208 +33 09 35.080388820   16.62 16.20     ~ 2820 2
8 LEDA 95597 LSB 06 47 45.6 +80 07 27   16.4       ~ 72 0
9 UGC 4483 GiG 08 37 03.00 +69 46 31.0 15.70 15.46 14.98 14.89   ~ 304 0
10 NAME F12D1 G 09 50 10.0 +67 30 24   15.6       ~ 55 1
11 LEDA 28529 G 09 53 48.8 +68 58 09   18.89       ~ 93 1
12 NAME M 81-82 Group GrG 09 55 +69.1           ~ 717 0
13 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4456 3
14 NAME Arp Loop G 09 57 29.0 +69 16 20           ~ 67 1
15 NAME Sextans B H2G 10 00 00.8217342072 +05 20 09.533389560 12.77 12.25 11.89 11.71   ~ 528 0
16 NGC 3109 AG? 10 03 06.877 -26 09 34.46 11.10 10.42 10.04 9.91   ~ 770 2
17 NAME Antlia Dwarf Galaxy G 10 04 03.9 -27 20 01 16.73 15.69 15.17 15.00   ~ 213 1
18 UGC 5428 AG? 10 05 06.40 +66 33 32.0 17.89 16.82 16.09 15.73   ~ 106 1
19 NAME Sex A H2G 10 11 00.5 -04 41 30 12.48 12.13 11.93 11.78   ~ 727 2
20 LEDA 4689216 GiG 10 21 25.2 +71 06 58           ~ 59 0
21 UGC 5692 GiG 10 30 35.03 +70 37 07.2 14.81 13.69 13.01 12.73   ~ 131 0
22 LEDA 32667 LSB 10 52 55.1 +69 32 46   17.2       ~ 86 1
23 NGC 3741 AG? 11 36 05.754 +45 17 02.96 15.01 14.55 14.23 14.06   ~ 220 0
24 UGC 6817 AG? 11 50 52.984 +38 52 50.92   13.72 13.9 13.39   ~ 166 0
25 NGC 4163 LSB 12 12 09.34 +36 10 08.1 14.33 13.70 13.2 12.98   ~ 222 0
26 NGC 4190 LSB 12 13 44.765 +36 38 02.49 13.88 13.40 13.25 12.86   ~ 211 0
27 UGCA 276 G 12 14 57.9 +36 13 07 17.66 16.85 16.22 15.92   ~ 100 1
28 Z 269-49 AG? 12 15 46.626 +52 23 13.91   15.3       ~ 70 0
29 UGC 7577 GiG 12 27 40.90 +43 29 44.0 13.75 13.10 12.7 12.33   ~ 255 0
30 NAME CVn I dwA GiC 12 38 40.06 +32 46 00.5 16.91 16.66 16.73 16.62   ~ 232 0
31 UGC 8091 H2G 12 58 40.1930636208 +14 13 00.739589628 15.24 15.16 14.98 14.81   ~ 463 0
32 UGC 8508 AG? 13 30 44.8682655624 +54 54 38.522749824 14.72 14.25 13.90 13.75   ~ 196 0
33 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4350 2
34 UGC 8651 AG? 13 39 53.75 +40 44 25.3 15.37 14.56 14.20 14.10   ~ 155 0
35 UGC 8760 AG? 13 50 51.3127548768 +38 01 14.958828876 15.56 14.78   14.33   ~ 148 0
36 LEDA 2807150 LSB 13 54 33.356 +04 14 39.66   16.8 17.1     ~ 84 0
37 UGC 8833 AG? 13 54 48.8114 +35 50 07.775   16.5   15.20   ~ 117 1
38 LEDA 166185 G 14 07 10.1 +35 03 37   16.9 17.2     ~ 90 0
39 UGC 9128 AG? 14 15 57.0834 +23 03 29.871 15.40 14.77 14.41 14.32   ~ 284 0
40 UGC 9240 AG? 14 24 43.21 +44 31 41.8 14.24 13.54 13.17 13.07   ~ 200 0
41 LEDA 2801026 LSB 16 13 47.504 +54 22 08.25     15.9     ~ 108 0
42 LEDA 2807157 GiG 23 45 35.177 +38 43 05.09   16.7 15.2     ~ 89 1
43 NAME Local Group GrG ~ ~           ~ 8415 0

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