2012MNRAS.427.3016P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.19CEST18:15:29

2012MNRAS.427.3016P - Mon. Not. R. Astron. Soc., 427, 3016-3028 (2012/December-3)

Discovery of planetary nebulae using predictive mid-infrared diagnostics.

PARKER Q.A., COHEN M., STUPAR M., FREW D.J., GREEN A.J., BOJICIC I., GUZMAN-RAMIREZ L., SABIN L. and VOGT F.

Abstract (from CDS):

We demonstrate a newly developed mid-infrared (MIR) planetary nebula (PN) selection technique. It is designed to enable efficient searches for obscured, previously unknown, PN candidates present in the photometric source catalogues of Galactic plane MIR sky surveys. Such selection is now possible via new, sensitive, high-to-medium resolution, MIR satellite surveys such as those from the Spitzer Space Telescope and the all-sky Wide-field Infrared Survey Explorer satellite missions. MIR selection is based on how different colour–colour planes isolate zones (sometimes overlapping) that are predominately occupied by different astrophysical object types. These techniques depend on the reliability of the available MIR source photometry. In this pilot study, we concentrate on MIR point-source detections and show that it is dangerous to take the MIR GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) photometry from Spitzer for each candidate at face value without examining the actual MIR image data. About half of our selected sources are spurious detections due to the applied source detection algorithms being affected by complex MIR backgrounds and the deblending of diffraction spikes around bright MIR point sources into point sources themselves. Nevertheless, once this additional visual diagnostic checking is performed, valuable MIR-selected PN candidates are uncovered. Four turned out to have faint, compact, optical counterparts in our Hα survey data missed in previous optical searches. We confirm all of these as true PNe via our follow-up optical spectroscopy. This lends weight to the veracity of our MIR technique. It demonstrates sufficient robustness that high-confidence samples of new Galactic PN candidates can be extracted from these MIR surveys without confirmatory optical spectroscopy and imaging. This is problematic or impossible when the extinction is large.

Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS

Journal keyword(s): H{sc ii} regions - planetary nebulae: general - infrared: ISM - radio continuum: general

Nomenclature: Fig. 1, Tables 2-3+6-7: GLIPN JHHMM+DDMM N=5.

Simbad objects: 42

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Number of rows : 42

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14984 1
2 SSTGLMC G295.4245+00.0434 PN? 11 47 02.981 -61 53 10.24           ~ 1 0
3 SSTGLMC G295.7630+00.7326 PN? 11 51 11.930 -61 17 52.28           ~ 1 0
4 WRAY 16-115 PN 12 28 46.8457795246 -63 44 37.072611293     15.70     ~ 54 0
5 SSTGLMC G302.0289-00.0561 PN? 12 43 30.256 -62 54 50.22           ~ 1 0
6 SSTGLMC G303.8027-00.1147 PN? 12 59 06.288 -62 58 24.77           ~ 1 0
7 SSTGLMC G305.3441-00.7489 PN? 13 13 06.043 -63 31 08.95           ~ 1 0
8 [RMB2008] G307.1055+00.6904 PN? 13 26 58.9302024554 -61 53 34.845362942           ~ 2 0
9 [RMB2008] G308.4962-00.1623 PN? 13 39 56.3765905221 -62 30 32.614638300           ~ 2 0
10 SSTGLMC G309.8085+00.6737 PN? 13 49 24.846 -61 25 17.54           ~ 1 0
11 SSTGLMC G311.8578+00.3703 PN? 14 06 34.192 -61 11 33.68           ~ 2 0
12 2MASS J14185145-6124377 Y*? 14 18 51.4378139290 -61 24 37.771528616           ~ 2 0
13 SSTGLMC G319.4987-00.4144 PN? 15 05 28.80744 -58 54 20.8404           ~ 2 0
14 SSTGLMC G322.6659+00.5251 PN? 15 22 06.851 -56 27 37.95           ~ 2 0
15 PN Pe 2-8 PN 15 23 42.8864008345 -57 09 25.223411201     15.50     ~ 71 0
16 SSTGLMC G323.9540+00.4384 PN? 15 30 08.723 -55 48 58.12           ~ 1 0
17 IRAS 15268-5547 PN 15 30 41.5847907209 -55 57 27.514292846           ~ 3 0
18 SSTGLMC G327.8259-00.8710 PN 15 57 15.528 -54 30 07.52           ~ 2 0
19 IRAS 15534-5422 PN 15 57 21.112 -54 30 46.13           ~ 11 0
20 SSTGLMC G330.3672-00.8723 PN? 16 10 07.224 -52 49 12.99           ~ 2 0
21 SSTGLMC G333.6931-00.3887 PN? 16 23 19.79712 -50 09 39.8232           ~ 2 0
22 SSTGLMC G335.2810-00.0084 PN? 16 28 28.208 -48 45 29.07           ~ 2 0
23 SSTGLMC G338.4491-00.0966 PN? 16 41 34.05120 -46 28 57.6840           ~ 2 0
24 SSTGLMC G339.7362+00.8468 PN 16 42 21.9827440248 -44 53 34.232049404           ~ 2 0
25 2MASS J17041916-4125101 IR 17 04 19.168 -41 25 10.17           ~ 1 0
26 SSTGLMC G345.9349+00.5487 PN? 17 04 54.955 -40 16 33.00           ~ 2 0
27 SSTGLMC G011.2060+00.8711 PN? 18 07 01.325 -18 48 45.15           ~ 1 0
28 SSTGLMC G010.5089-00.6242 PN? 18 11 08.404 -20 08 48.27           ~ 1 0
29 SSTGLMC G012.5223-01.0139 PN? 18 16 40.455 -18 33 54.76           ~ 1 0
30 SSTGLMC G019.5325+00.7308 PN 18 23 59.985 -11 33 39.29           ~ 3 0
31 SSTGLMC G025.7769+00.8167 PN? 18 35 24.887 -05 59 21.02           ~ 1 0
32 SSTGLMC G023.2256-00.5250 PN? 18 35 29.106 -08 52 18.10           ~ 1 0
33 UGPS J184303.28-041719.0 PN? 18 43 03.282 -04 17 19.00           ~ 2 0
34 SSTGLMC G039.0344-00.2058 PN? 19 03 20.236 +05 20 04.92           ~ 1 0
35 2MASS J19064427+0704498 Y*O 19 06 44.272 +07 04 49.83           ~ 3 0
36 SSTGLMC G056.1486+00.4087 PN? 19 34 10.70784 +20 44 14.7336           ~ 2 0
37 PN K 3-42 PN 19 39 35.785 +20 19 01.87           ~ 29 0
38 2MASS J19393603+2019072 IR 19 39 36.030 +20 19 07.24           ~ 1 0
39 SSTGLMC G060.0271+00.6070 PN? 19 41 39.419 +24 12 56.25           ~ 1 0
40 * 42 Peg PM* 22 41 27.7207176 +10 49 52.907917 3.10 3.33 3.41 3.43 3.50 B8V 282 0
41 LP 877-23 PM* 22 52 41.0353308036 -20 35 32.995847106   13.02 11.90     ~ 104 0
42 NAME Galactic Bulge reg ~ ~           ~ 3454 0

    Equat.    Gal    SGal    Ecl

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2020.10.19-18:15:29

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