2015A&A...582A..28P

Query : 2015A&A...582A..28P

2015A&A...582A..28P - Astronomy and Astrophysics, volume 582A, 28-28 (2015/10-1)

Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BANDAY A.J., BARREIRO R.B., BARTOLO N., BATTANER E., BATTYE R., BENABED K., BENDO G.J., BENOIT-LEVY A., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BONALDI A., BONAVERA L., BOND J.R., BORRILL J., BOUCHET F.R., BURIGANA C., BUTLER R.C., CALABRESE E., CARDOSO J.-F., CATALANO A., CHAMBALLU A., CHARY R.-R., CHEN X., CHIANG H.C., CHRISTENSEN P.R., CLEMENTS D.L., 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., 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., FINELLI F., FORNI O., FRAILIS M., FRAISSE A.A., FRANCESCHI E., FREJSEL A., GALEOTTA S., GANGA K., GIARD M., GIRAUD-HERAUD Y., GJERLOW E., GONZALEZ-NUEVO J., GORSKI K.M., GREGORIO A., GRUPPUSO A., HANSEN F.K., HANSON D., HARRISON D.L., 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., ISRAEL F.P., JAFFE A.H., JAFFE T.R., JONES W.C., JUVELA M., KEIHAENEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAEHTEENMAEKI A., LAMARRE J.-M., LASENBY A., LATTANZI M., LAWRENCE C.R., LEONARDI R., LEVRIER F., LIGUORI M., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUBIN P.M., MACIAS-PEREZ J.F., MADDEN S., MAFFEI B., MAINO D., MANDOLESI N., MARIS M., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MATARRESE S., MAZZOTTA P., MENDES L., MENNELLA A., MIGLIACCIO M., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MUNSHI D., MURPHY J.A., 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., PARTRIDGE B., PASIAN F., PEARSON T.J., PEEL M., PERDEREAU O., PERROTTA F., PETTORINO V., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., POPA L., PRATT G.W., PRUNET S., PUGET J.-L., RACHEN J.P., REINECKE M., REMAZEILLES M., RENAULT C., RICCIARDI S., RISTORCELLI I., ROCHA G., ROSSET C., ROSSETTI M., ROUDIER G., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SAVINI G., SCOTT D., SPENCER L.D., STOLYAROV V., SUDIWALA R., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TRISTRAM M., TUCCI M., UMANA G., VALENZIANO L., VALIVIITA J., VAN TENT B., VIELVA P., VILLA F., WADE L.A., WANDELT B.D., WATSON R., WEHUS I.K., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

The Andromeda galaxy (M31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiral arms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M31. We find that dust dominating the longer wavelength emission (>0.3mm) is heated by the diffuse stellar population (as traced by 3.6µm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24µm emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22K in the nucleus to 14K outside of the 10kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2±1.0)K, with a spectral index of 1.62±0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60GHz, which corresponds to a star formation rate of around 0.12M_☉/yr. We find a 2.3σ detection of the presence of spinning dust emission, with a 30GHz amplitude of 0.7±0.3Jy, which is in line with expectations from our Galaxy.

Abstract Copyright: ∼

Journal keyword(s): galaxies: individual: Messier 31 - galaxies: structure - galaxies: ISM - submillimeter: galaxies - radio continuum: galaxies

Simbad objects: 15

Full paper

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Number of rows : 15

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	5C 3.50	QSO	00 38 24.84358446	+41 37 06.0002701		19.9	19.9	18.95		~	133	1
2	M 110	GiG	00 40 22.0572349992	+41 41 07.507220136		8.92	8.07			~	1296	1
3	BD+40 147	IG	00 42 41.825	+40 51 54.61	9.51	9.03	8.08			~	2135	2
4	M 31	G	00 42 44.330	+41 16 07.50	4.86	4.36	3.44			~	12390	1
5	NGC 253	SyG	00 47 33.134	-25 17 19.68		8.03		6.94	8.1	~	3262	2
6	NAME SMC	G	00 52 38.0	-72 48 01		2.79	2.2			~	10857	1
7	M 33	GiG	01 33 50.8965749232	+30 39 36.630403128	6.17	6.27	5.72			~	5729	1
8	M 74	G	01 36 41.7451236624	+15 47 01.107512304	10.52	10.00	9.46	9.16		~	1679	1
9	NAME LMC	G	05 23 34.6	-69 45 22			0.4			~	17000	1
10	NGC 2403	AGN	07 36 51.3381434280	+65 36 09.650825640	9.31	8.84	8.38	8.19		~	1758	1
11	M 81	Sy2	09 55 33.1726556496	+69 03 55.062505368		7.89	6.94			~	4360	3
12	M 82	IG	09 55 52.430	+69 40 46.93	9.61	9.30	8.41			~	5767	6
13	NGC 4945	Sy2	13 05 27.279	-49 28 04.44		9.31	14.40	7.55		~	1437	2
14	M 83	SBG	13 37 00.91920	-29 51 56.7400	8.85	8.11	7.52	7.21		~	2520	2
15	NGC 6946	H2G	20 34 52.332	+60 09 13.24		10.5				~	2475	2

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