2014A&A...565A.103P

Query : 2014A&A...565A.103P

2014A&A...565A.103P - Astronomy and Astrophysics, volume 565A, 103-103 (2014/5-1)

Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ALVES M.I.R., ARNAUD M., ATRIO-BARANDELA F., AUMONT J., BACCIGALUPI C., BANDAY A.J., BARREIRO R.B., BATTANER E., BENABED K., BENOIT-LEVY A., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BOBIN J., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BURIGANA C., CARDOSO J.-F., CASASSUS S., CATALANO A., CHAMBALLU A., CHEN X., CHIANG H.C., CHIANG L.-Y., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBI S., COLOMBO L.P.L., COUCHOT F., CRILL B.P., CUTTAIA F., DANESE L., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DESERT F.-X., DICKINSON C., DIEGO J.M., DONZELLI S., DORE O., DUPAC X., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FORNI O., FRANCESCHI E., GALEOTTA S., GANGA K., GENOVA-SANTOS R.T., GHOSH T., GIARD M., GONZALEZ-NUEVO J., GORSKI K.M., GREGORIO A., GRUPPUSO A., HANSEN F.K., HARRISON D.L., HELOU G., HERNANDEZ-MONTEAGUDO C., HILDEBRANDT S.R., HIVON E., HOBSON M., HORNSTRUP A., JAFFE A.H., JAFFE T.R., JONES W.C., KEIHAENEN E., KESKITALO R., KNEISSL R., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAEHTEENMAEKI A., LAMARRE J.-M., LASENBY A., LAWRENCE C.R., LEONARDI R., LIGUORI M., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., MACIAS-PEREZ J.F., MAFFEI B., MAINO D., MANDOLESI N., MARSHALL D.J., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MAZZOTTA P., MEINHOLD P.R., MELCHIORRI A., MENDES L., MENNELLA A., MIGLIACCIO M., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MUNSHI D., NASELSKY P., NATI F., NATOLI P., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., OXBORROW C.A., PAGANO L., PAJOT F., PALADINI R., PAOLETTI D., PATANCHON G., PEARSON T.J., PEEL M., PERDEREAU O., PERROTTA F., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., PONTHIEU N., POPA L., PRATT G.W., PRUNET S., PUGET J.-L., RACHEN J.P., REBOLO R., REICH W., REINECKE M., REMAZEILLES M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., ROUDIER G., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SAVINI G., SCOTT D., SPENCER L.D., STOLYAROV V., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TAVAGNACCO D., TERENZI L., TIBBS C.T., TOFFOLATTI L., TOMASI M., TRISTRAM M., TUCCI M., VALENZIANO L., VALIVIITA J., VAN TENT B., VARIS J., VERSTRAETE L., VIELVA P., VILLA F., WANDELT B.D., WATSON R., WILKINSON A., YSARD N., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1°-smoothed maps from 0.408GHz up to 3000GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5σ) excess emission at frequencies between 20 and 60GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact HII regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20-35GHz except for the California nebula (NGC1499), which appears to have a high spinning dust peak frequency of (50±17)GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20K and an average emissivity index, βd, of +1.8, while the non-AME regions are typically warmer, at 20-27K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G0. Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with HII regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12µm/25µm ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase.

Abstract Copyright: ∼

Journal keyword(s): HII regions - radiation mechanisms: general - radio continuum: ISM - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/A+A/565/A103): table3.dat>

Errata: erratum vol. 610, art. C1 (2018)

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

CDS comments: Paragraph 4.2 PMN J0805-0438 not identifed.

Simbad objects: 123

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Number of rows : 123
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 7822 HII 00 01 08.58 +67 25 17.0           ~ 118 3
2 NGC 281 HII 00 52 25.1 +56 33 54           ~ 242 1
3 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 1032 3
4 LDN 1358 DNe 02 55 54 +69 20.8           ~ 11 0
5 TGU H942 DNe 03 27.3 +58 33           ~ 8 0
6 LDN 1450 DNe 03 29.6 +31 20           ~ 61 0
7 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1364 0
8 Cl Melotte 22 OpC 03 46 24.2 +24 06 50           ~ 3434 0
9 * ksi Per ** 03 58 57.9024302099 +35 47 27.709515737 3.190 4.080 4.060 3.88 3.89 O7.5III(n)((f)) 832 0
10 NGC 1499 HII 04 03 18 +36 25.3           ~ 170 0
11 SH 2-209 HII 04 11 06.7 +51 09 44           ~ 96 0
12 NGC 1893 OpC 05 22 53.8 +33 26 38           ~ 261 0
13 LDN 1582 DNe 05 32 00.3 +12 30 28           ~ 20 0
14 M 42 HII 05 35 17 -05 23.4           ~ 4074 0
15 SH 2-235 HII 05 41.1 +35 50           ~ 218 0
16 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 375 0
17 SH 2-242 HII 05 51 54.8 +27 01 56           ~ 53 1
18 LDN 1622 DNe 05 54 28 +01 48.2           ~ 104 0
19 LDN 1621 DNe 05 55.0 +02 20           ~ 13 0
20 LDN 1557 DNe 06 06.2 +30 00           ~ 10 0
21 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 742 2
22 NGC 2170 RNe 06 07 48 -06 23.1           ~ 43 0
23 NGC 2174 HII 06 09.7 +20 30           ~ 22 1
24 IC 2162 HII 06 13 04.1 +17 58 44           ~ 358 2
25 TGU H1544 DNe 06 29.0 -10 00           ~ 3 0
26 LBN 1015 RNe 06 30 -09.6           ~ 6 0
27 LBN 970 HII 06 34 22 +02 28.1           ~ 21 0
28 LDN 1608 DNe 06 36 37.2 +10 44 26           ~ 5 0
29 LDN 1613 DNe 06 40.7 +09 27           ~ 11 0
30 NAME Cone Nebula DNe 06 41.1 +09 53           ~ 86 1
31 LBN 211.65-01.51 HII 06 45 28 +00 17.8           ~ 67 0
32 LDN 1650 DNe 06 59.5 -04 54           ~ 10 0
33 TGU H1630 DNe 07 09.3 -36 27           ~ 3 0
34 TGU H1593 DNe 07 18.7 -17 41           ~ 2 0
35 V* VY CMa s*r 07 22 58.3261352189 -25 46 03.194390594 12.01 10.068 8.691 7.938   M5Iae 1103 0
36 LBN 1059 HII 07 24 04.8 -25 58 15           ~ 21 0
37 LDN 1667 DNe 07 25.1 -25 46           ~ 12 0
38 BRAN 34 ISM 07 29 29.1 -47 04 13           ~ 3 0
39 LBN 1050 HII 07 31 02.4 -19 09 17           ~ 23 1
40 TGU H1667 DNe 07 31.1 -46 59           ~ 2 0
41 NAME GUM Nebula ISM 07 43 -42.1           ~ 421 1
42 NGC 2467 OpC 07 52 18 -26 25.7           ~ 185 1
43 TGU H1811 DNe 07 58.3 -80 56           ~ 2 0
44 BRAN 124A RNe 08 14 50.4 -35 55 23           ~ 7 0
45 GUM 10 HII 08 16 16.8 -35 37 58           ~ 32 0
46 BRAN 166 HII 08 38 08.0 -40 17 53           ~ 29 1
47 RCW 36 HII 08 59 00.9 -43 44 10     15.20     ~ 147 0
48 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 305 2
49 TYC 8170-333-1 HII 09 16 58.2089265600 -47 57 47.393035668   13.36 12.96     ~ 23 0
50 BRAN 261 RNe 09 23 59.5 -51 44 14           ~ 4 0
51 GUM 26 HII 09 24 30.1 -51 59 07           ~ 45 0
52 RCW 46 HII 10 06 39 -57 12.2           ~ 18 0
53 GUM 29 HII 10 24 14.6 -57 46 58           ~ 210 0
54 NGC 3247 OpC 10 25 52 -57 55.6   7.99 7.6     ~ 38 0
55 NGC 3372 HII 10 45 02.23 -59 41 59.8           ~ 1014 2
56 GUM 35 HII 10 58 50.9 -61 06 38           ~ 14 0
57 BRAN 337 HII 11 02 56.1 -59 29 16           ~ 17 0
58 RCW 57 HII 11 14.7 -61 12           ~ 15 0
59 NGC 3603 OpC 11 15 10.8 -61 15 32           ~ 1065 1
60 IC 2944 OpC 11 38 20.00 -63 22 22.0           ~ 184 0
61 [KC97c] G298.6-00.1 HII 12 13 12.6 -62 39 39           ~ 12 0
62 GRS G305.40 +00.20 HII 13 10 19 -62 38.5           ~ 33 0
63 GRS G311.89 +00.10 HII 14 07 35.2 -61 27 18           ~ 29 1
64 GAL 317.60-00.36 HII 14 52 07.3 -59 45 13           ~ 5 0
65 GAL 320.23-00.29 HII 15 09 53.4 -58 25 40           ~ 16 0
66 TGU H1978 DNe 15 13.4 -62 44           ~ 2 0
67 GN 15.11.0 RNe 15 15 06 -62 45.8           ~ 2 0
68 GAL 322.16+00.62 HII 15 18 39.1 -56 38 49           ~ 29 0
69 LDN 1780 DNe 15 39.7 -07 10           ~ 80 0
70 MBM 121 MoC 15 40.6 -24 57           ~ 2 0
71 RCW 97 HII 15 53 05.0 -54 35 24           ~ 157 0
72 LDN 134 MoC 15 53 36.3 -04 35 26           ~ 208 0
73 [VV2006] J155530.8-032650 QSO 15 55 30.74814773 -03 26 49.5200171     20.7 19.9   ~ 28 1
74 LBN 1105 HII 16 20 -25.3           ~ 1 0
75 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3629 1
76 SNR G337.0-00.1 SNR 16 35 06.9 -47 47 25           ~ 130 1
77 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2191 0
78 LDN 137 DNe 16 50.9 -15 25           ~ 9 0
79 GAL 343.4-00.0 HII 16 59 16 -42 36.4           ~ 2 0
80 RCW 117 HII 17 09 34.0 -41 36 12           ~ 67 2
81 BFS 65 HII 17 20 06.9 -38 57 34           ~ 78 0
82 NGC 6357 OpC 17 24 44 -34 12.2           ~ 274 0
83 Kes 52 Rad 17 29 15 -36 40.0           ~ 5 0
84 SNR G355.6+00.0 SNR 17 35 18 -32 37.0           ~ 27 0
85 SNR G008.3-00.0 Rad 18 04.6 -21 49           ~ 25 1
86 LDN 462 DNe 18 07 33 -04 41.7           ~ 12 0
87 Kes 62 Rad 18 09 22 -20 19.3           ~ 4 0
88 SNR G009.9-00.8 SNR 18 10.7 -20 43           ~ 19 0
89 SNR G012.8-00.2 SFR 18 14 14.0 -17 55 50           ~ 256 0
90 M 16 OpC 18 18 45.1 -13 47 31           ~ 1028 1
91 W 37 Rad 18 18 50.1 -13 46 44           ~ 25 1
92 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1612 0
93 LBN 028.77+03.43 HII 18 31 26.5 -02 04 22           ~ 230 2
94 RCW 175 HII 18 46.8 -03 45           ~ 27 0
95 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 531 0
96 CTB 61 HII 18 56.4 +07 55           ~ 10 0
97 CTB 64 Rad 19 00 59 +04 14.2           ~ 42 0
98 SNR G035.2-01.8 SNR 19 01.6 +01 14           ~ 153 0
99 W 49 SFR 19 10 20 +09 07.7           ~ 575 1
100 SNR G045.5+00.1 SNR 19 14 20 +11 09.1           ~ 12 0
101 LMH 51 Rad 19 29.3 +18 12           ~ 11 0
102 LBN 059.38-00.15 HII 19 43 12 +23 15.0           ~ 22 1
103 LBN 061.50+00.29 HII 19 46 45.7 +25 12 56           ~ 66 0
104 SH 2-89 HII 19 50 04.5 +26 28 23   13.72 12.11     ~ 13 0
105 LBN 068.07+00.92 HII 19 59 01 +31 22.5   14.25 13.53     ~ 26 0
106 LBN 071.58+02.86 HII 19 59 55 +35 16.6           ~ 35 0
107 SH 2-105 HII 20 21 38.2 +37 31 11           ~ 20 0
108 GAL 075.84+00.40 HII 20 21 38.3 +37 31 12           ~ 25 0
109 SH 2-106 HII 20 27 26.8 +37 22 49           ~ 440 1
110 NAME Cyg X BL? 20 30 04.7973633 +40 51 36.002197           ~ 843 1
111 DR 23 Rad 20 40.8 +41 54           ~ 40 0
112 GAL 093.06+02.81 HII 21 12 21.1 +52 28 59           ~ 30 0
113 LBN 094.79-01.77 HII 21 38 26 +50 23.1           ~ 38 0
114 IC 1396 OpC 21 38 58.8 +57 30 50           ~ 496 1
115 LDN 1111 DNe 21 40 30.0 +57 48 00           ~ 16 0
116 LDN 1059 DNe 21 40 57.422 +50 39 58.32           ~ 14 0
117 TGU H582 DNe 21 41.4 +54 57           ~ 2 0
118 GM 1-12 RNe 21 42 22.0 +54 54 45           ~ 13 0
119 LDN 1161 DNe 22 19.9 +56 08           ~ 4 0
120 LBN 110.11+02.44 HII 22 57 06 +62 38.2           ~ 103 0
121 TGU H684 DNe 22 57.4 +59 28           ~ 2 0
122 SH 2-152 HII 22 58 40.8107767416 +58 46 59.226036024           ~ 138 1
123 NAME Gould Belt PoG ~ ~           ~ 873 1

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