CDS

2016A&A...594A..25P

Query : 2016A&A...594A..25P

2016A&A...594A..25P - Astronomy and Astrophysics, volume 594A, 25-25 (2016/10-1)

Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ALVES M.I.R., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BARTOLO N., BATTANER E., BENABED K., BENOIT A., BENOIT-LEVY A., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BOCK J.J., BONALDI A., BONAVERA L., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BUCHER M., BURIGANA C., BUTLER R.C., CALABRESE E., CARDOSO J.-F., CATALANO A., CHALLINOR A., CHAMBALLU A., CHARY R.-R., CHIANG H.C., CHRISTENSEN P.R., COLOMBI S., COLOMBO L.P.L., COMBET C., COUCHOT F., COULAIS A., CRILL B.P., CURTO A., CUTTAIA F., DANESE L., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DESERT F.-X., DICKINSON C., DIEGO J.M., DOLE H., DONZELLI S., DORE O., DOUSPIS M., DUCOUT A., DUPAC X., EFSTATHIOU G., ELSNER F., ENSSLIN T.A., ERIKSEN H.K., FALGARONE E., FERGUSSON J., FINELLI F., FORNI O., FRAILIS M., FRAISSE A.A., FRANCESCHI E., FREJSEL A., GALEOTTA S., GALLI S., GANGA K., GHOSH T., GIARD M., GIRAUD-HERAUD Y., GJERLOW E., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., GUDMUNDSSON J.E., HANSEN F.K., HANSON D., HARRISON D.L., HELOU G., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOVEST W., HUFFENBERGER K.M., HURIER G., JAFFE A.H., JAFFE T.R., JONES W.C., JUVELA M., KEIHANEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAHTEENMAKI A., LAMARRE J.-M., LASENBY A., LATTANZI M., LAWRENCE C.R., LEAHY J.P., LEONARDI R., LESGOURGUES J., LEVRIER F., LIGUORI M., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUBIN P.M., MACIAS-PEREZ J.F., MAGGIO G., MAINO D., MANDOLESI N., MANGILLI A., MARIS M., MARSHALL D.J., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MATARRESE S., McGEHEE P., MEINHOLD P.R., MELCHIORRI A., MENDES L., MENNELLA A., MIGLIACCIO M., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MOSS A., MUNSHI D., MURPHY J.A., NATI F., NATOLI P., NETTERFIELD C.B., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., ORLANDO E., OXBORROW C.A., PACI F., PAGANO L., PAJOT F., PALADINI R., PAOLETTI D., PARTRIDGE B., PASIAN F., PATANCHON G., PEARSON T.J., PEEL M., PERDEREAU O., PEROTTO L., PERROTTA F., PETTORINO V., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., PRATT G.W., PREZEAU G., PRUNET S., PUGET J.-L., RACHEN J.P., REACH W.T., REBOLO R., REINECKE M., REMAZEILLES M., RENAULT C., RENZI A., RISTORCELLI I., ROCHA G., ROSSET C., ROSSETTI M., ROUDIER G., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SANTOS D., SAVELAINEN M., SAVINI G., SCOTT D., SEIFFERT M.D., SHELLARD E.P.S., SPENCER L.D., STOLYAROV V., STOMPOR R., STRONG A.W., SUDIWALA R., SUNYAEV R., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TRISTRAM M., TUCCI M., TUOVINEN J., UMANA G., VALENZIANO L., VALIVIITA J., VAN TENT F., VIDAL M., VIELVA P., VILLA F., WADE L.A., WANDELT B.D., WATSON R., WEHUS I.K., WILKINSON A., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

We discuss the Galactic foreground emission between 20 and 100GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude Hα emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (~=30%) of Hα having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in Iν) ranging from below 20GHz to more than 50GHz. There is a strong tendency for the spinning dust component near many prominent HII regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5-20GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40°>l>-90° is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the "Fermi bubble/microwave haze", making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20deg long filament seen in Hα at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2σ upper limit of 1.6% in the Perseus region.

Abstract Copyright: © ESO, 2016

Journal keyword(s): diffuse radiation - ISM: general - radiation mechanisms: general - radio continuum: ISM - polarization - local insterstellar matter

Simbad objects: 69

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Number of rows : 69
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023 		#notes
1 NAME NCP reg 00 00 00 +90 00.0           ~ 169 0
2 NAME SGP reg 00 51 26.275 -27 07 41.70           ~ 556 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10598 1
4 NAME Loop III SR? 01 12 +78.3           ~ 88 1
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6625 1
6 NAME Per Arm PoG 03 30 +45.0           ~ 1443 0
7 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1279 0
8 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 260 0
9 NGC 1499 HII 04 03 18 +36 25.3           ~ 168 0
10 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 194 0
11 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4134 0
12 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16630 1
13 NAME Barnard's Loop HII 05 27.5 -03 58           ~ 120 1
14 NAME lam Ori Complex SFR 05 35 06 +09 56.0           ~ 76 0
15 * lam Ori ** 05 35 08.27761 +09 56 02.9611 2.45 3.48 3.66 3.72 3.89 O8IIIf+B0.5V 292 0
16 M 42 OpC 05 35 17 -05 23.4           ~ 3982 0
17 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 556 0
18 NAME Ori Complex Cld 05 35.3 -05 23           ~ 410 0
19 NAME lam Ori Molecular Ring HII 05 35.3 +09 56           ~ 75 1
20 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 221 0
21 NAME Ori A MoC 05 38 -07.1           ~ 2913 0
22 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1141 2
23 NGC 2070 Cl* 05 38 42 -69 06.0     7.25     ~ 361 1
24 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1923 1
25 LDN 1641 MoC 05 39.0 -07 00           ~ 468 0
26 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1311 0
27 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 366 0
28 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1038 1
29 NAME GUM Nebula ISM 07 43 -42.1           ~ 414 1
30 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1201 2
31 * rho01 Cnc PM* 08 52 35.8111044043 +28 19 50.954994470 7.45 6.82   5.4   K0IV-V 1069 1
32 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 185 1
33 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1099 1
34 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 765 0
35 NAME North Polar Spur ISM 12 00 +00.0           ~ 348 1
36 NAME Musca Cld 12 23 -71.3           ~ 202 0
37 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6417 0
38 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5652 1
39 NAME Cha II MoC 12 54 -77.2           ~ 322 0
40 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4629 2
41 NAME Loop IV SNR 13 24 -13.6           ~ 57 1
42 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4344 3
43 NAME Loop I SR? 15 01 -38.7           ~ 367 2
44 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1275 1
45 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3478 1
46 LBN 006.00+24.73 HII 16 35 56.8 -12 43 05           ~ 59 0
47 NAME Fermi Bubbles bub 17 45 -29.0           ~ 382 0
48 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13551 0
49 NAME NEP reg 18 00 00.000 +66 33 38.55           ~ 325 0
50 NAME Aql Rift DNe 18 32 -01.0           ~ 303 1
51 RCW 175 HII 18 46.8 -03 45           ~ 26 0
52 V* TY CrA Ae* 19 01 40.8284458320 -36 52 33.816176040 10.03 9.92 9.39     B9e 279 0
53 NGC 6729 ISM 19 01 46.4 -36 57 40           ~ 54 0
54 NAME Corona Australis Cloud MoC 19 01 51 -36 58.9           ~ 459 0
55 V* R CrA Ae* 19 01 53.6764322232 -36 57 08.299341828 12.781 12.651 11.917 11.242 10.412 B5IIIpe 472 1
56 NAME Loop VIIb Rad 19 29 -38.0           ~ 10 1
57 SNR G068.8+02.6 SNR 19 52 55 +32 54.2           ~ 347 1
58 SNR G074.9+01.2 SNR 20 16 01.8 +37 12 53           ~ 178 2
59 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 765 1
60 NAME Cyg Loop SNR 20 51.0 +30 40           ~ 887 0
61 MBM 53 MoC 23 08 07.3 +22 56 15           ~ 47 0
62 [DB2002b] G89.19-40.94 MoC 23 08 24 +15 05.3           ~ 84 0
63 SH 2-122 HII 23 08.8 +14 55           ~ 8 0
64 NAME Loop 2 SR? 23 25 +26.5           ~ 77 1
65 NAME Galactic Ridge ? ~ ~           ~ 478 1
66 NAME MBM 53-55 Cld ~ ~           ~ 19 0
67 NAME Gould Belt PoG ~ ~           ~ 842 1
68 NAME SCP reg ~ ~           ~ 88 0
69 NAME Polar Spur SNR ~ ~           ~ 10 0

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2023.03.23-21:25:17

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