2011A&A...536A..25P

Query : 2011A&A...536A..25P

2011A&A...536A..25P - Astronomy and Astrophysics, volume 536A, 25-25 (2011/12-1)

Planck early results. XXV. Thermal dust in nearby molecular clouds.

PLANCK COLLABORATION, ABERGEL A., ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BALBI A., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BATTANER E., BENABED K., BENOIT A., BERNARD J.-P., BERSANELLI M., BHATIA R., BOCK J.J., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BUCHER M., BURIGANA C., CABELLA P., CARDOSO J.-F., CATALANO A., CAYON L., CHALLINOR A., CHAMBALLU A., CHIANG L.-Y., CHIANG C., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBI S., COUCHOT F., COULAIS A., CRILL B.P., CUTTAIA F., DANESE L., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE GASPERIS G., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DESERT F.-X., DICKINSON C., DOBASHI K., DONZELLI S., DORE O., DOERL U., DOUSPIS M., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FORNI O., FRAILIS M., FRANCESCHI E., GALEOTTA S., GANGA K., GIARD M., GIARDINO G., GIRAUD-HERAUD Y., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., GUILLET V., HANSEN F.K., HARRISON D., HENROT-VERSILLE S., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HOVEST W., HOYLAND R.J., HUFFENBERGER K.M., JAFFE A.H., JONES A., JONES W.C., JUVELA M., KEIHAENEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOX L., KURKI-SUONIO H., LAGACHE G., LAMARRE J.-M., LASENBY A., LAUREIJS R.J., LAWRENCE C.R., LEACH S., LEONARDI R., LEROY C., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUBIN P.M., MACIAS-PEREZ J.F., MacTAVISH C.J., MAFFEI B., MANDOLESI N., MANN R., MARIS M., MARSHALL D.J., MARTIN P., MARTINEZ-GONZALEZ E., MASI S., MATARRESE S., MATTHAI F., MAZZOTTA P., McGEHEE P., MEINHOLD P.R., MELCHIORRI A., MENDES L., MENNELLA A., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MUNSHI D., MURPHY A., NASELSKY P., NATOLI P., NETTERFIELD C.B., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., OSBORNE S., PAJOT F., PALADINI R., PASIAN F., PATANCHON G., PERDEREAU O., PEROTTO L., PERROTTA F., PIACENTINI F., PIAT M., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., PONTHIEU N., POUTANEN T., PREZEAU G., PRUNET S., PUGET J.-L., REACH W.T., REBOLO R., REINECKE M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SANTOS D., SAVINI G., SCOTT D., SEIFFERT M.D., SHELLARD P., SMOOT G.F., STARCK J.-L., STIVOLI F., STOLYAROV V., SUDIWALA R., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TORRE J.-P., TRISTRAM M., TUOVINEN J., UMANA G., VALENZIANO L., VERSTRAETE L., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

Planck allows unbiased mapping of Galactic sub-millimetre and millimetre emission from the most diffuse regions to the densest parts of molecular clouds. We present an early analysis of the Taurus molecular complex, on line-of-sight-averaged data and without component separation. The emission spectrum measured by Planck and IRAS can be fitted pixel by pixel using a single modified blackbody. Some systematic residuals are detected at 353GHz and 143GHz, with amplitudes around -7% and +13%, respectively, indicating that the measured spectra are likely more complex than a simple modified blackbody. Significant positive residuals are also detected in the molecular regions and in the 217 GHz and 100 GHz bands, mainly caused by the contribution of the J=2->1 and J=1->0 ¹²CO and ¹³CO emission lines. We derive maps of the dust temperature T, the dust spectral emissivity index β, and the dust optical depth at 250τ₂₅₀. The temperature map illustrates the cooling of the dust particles in thermal equilibrium with the incident radiation field, from 16-17 K in the diffuse regions to 13-14 K in the dense parts. The distribution of spectral indices is centred at 1.78, with a standard deviation of 0.08 and a systematic error of 0.07. We detect a significant T-β anti-correlation. The dust optical depth map reveals the spatial distribution of the column density of the molecular complex from the densest molecular regions to the faint diffuse regions. We use near-infrared extinction and HI data at 21-cm to perform a quantitative analysis of the spatial variations of the measured dust optical depth at 250µm per hydrogen atom τ₂₅₀/N_H. We report an increase of τ₂₅₀/N_H by a factor of about 2 between the atomic phase and the molecular phase, which has a strong impact on the equilibrium temperature of the dust particles.

Abstract Copyright: ∼

Journal keyword(s): dust, extinction - ISM: structure - evolution - infrared: ISM - ISM: individual objects: Taurus-Auriga molecular cloud

Simbad objects: 7

Full paper

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Number of rows : 7

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Sp type	#ref 1850 - 2023	#notes
1	NAME Perseus Cloud	SFR	03 35.0	+31 13	~	1311	0
2	NAME Per Region	reg	03 37 00.0	+31 15 00	~	264	0
3	NAME Tau-Aur Complex	SFR	04 30	+25.0	~	1338	0
4	NAME Kutner's Cloud	MoC	04 32 44.6	+24 23 13	~	268	0
5	NAME [BM89] TMC-2	PoC	04 32 44.7	+24 25 13	~	186	0
6	NAME Taurus Complex	SFR	04 41.0	+25 52	~	4248	0
7	NAME Polaris Flare	MoC	11 00 14.8	+86 10 52	~	186	1

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