Herschel-ATLAS: statistical properties of Galactic cirrus in the GAMA-9 Hour Science Demonstration Phase Field

被引：45

作者：

Bracco, A. ^{[1
]}

Cooray, A. ^{[1
,2
]}

Veneziani, M. ^{[1
,3
]}

Amblard, A. ^{[1
]}

Serra, P. ^{[1
]}

Wardlow, J. ^{[1
]}

Thompson, M. A. ^{[4
]}

White, G. ^{[5
,6
]}

Auld, R. ^{[7
]}

Baes, M. ^{[8
]}

Bertoldi, F. ^{[9
]}

Buttiglione, S. ^{[10
]}

Cava, A. ^{[11
,12
]}

Clements, D. L. ^{[13
]}

Dariush, A. ^{[7
]}

De Zotti, G. ^{[10
,14
]}

Dunne, L. ^{[15
]}

Dye, S. ^{[7
]}

Eales, S. ^{[7
]}

Fritz, J. ^{[8
]}

Gomez, H. ^{[7
]}

Hopwood, R. ^{[5
]}

Ibar, I. ^{[16
]}

Ivison, R. J. ^{[16
,17
]}

Jarvis, M. ^{[4
]}

Lagache, G. ^{[18
,19
]}

Lee, M. G. ^{[20
]}

Leeuw, L. ^{[21
]}

Maddox, S. ^{[15
]}

Michalowski, M. ^{[17
]}

Pearson, C. ^{[5
,22
,23
]}

Pohlen, M. ^{[7
]}

Rigby, E. ^{[15
]}

Rodighiero, G. ^{[24
]}

Smith, D. J. B. ^{[15
]}

Temi, P. ^{[25
]}

Vaccari, M. ^{[24
]}

van der Werf, P. ^{[17
,26
]}

机构：

[1] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[2] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[3] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[4] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England

[5] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

[6] Rutherford Appleton Lab, Space Sci & Technol Div, Chilton OX11 0NL, Oxon, England

[7] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[8] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium

[9] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[10] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany

[11] Univ La Laguna, Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain

[12] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain

[13] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Dept Phys, London SW7 2AZ, England

[14] SISSA, I-34136 Trieste, Italy

[15] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[16] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[17] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[18] Univ Paris 11, Lab IAS, UMR8617, F-91405 Orsay, France

[19] CNRS, F-91405 Orsay, France

[20] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea

[21] SETI Inst, Mountain View, CA 94043 USA

[22] Rutherford Appleton Lab, Space Sci & Technol Dept, Chilton OX11 0QX, Oxon, England

[23] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada

[24] Univ Padua, Dept Astron, Padua, Italy

[25] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA

[26] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 412卷 / 02期

关键词：

methods: statistical; ISM: structure; infrared: ISM; TEMPERATURE-DEPENDENCE; SPECTRAL INDEX; ABSORPTION-COEFFICIENT; SPIRE INSTRUMENT; NUMBER COUNTS; DUST EMISSION; MICRONS; NOISE; GRAINS; CORES;

D O I：

10.1111/j.1365-2966.2010.17971.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the spectral energy distribution (SED) and the power spectrum of Galactic cirrus emission observed in the 14 deg2 Science Demonstration Phase field of the Herschel-ATLAS using Herschel and IRAS data from 100 to 500 mu m. We compare the Spectral and Photometric Imaging Receiver (SPIRE) 250, 350 and 500 mu m maps with IRAS 100-mu m emission, binned in 6-arcmin pixels. We assume a modified blackbody SED with dust emissivity parameter beta (F proportional to lambda-beta) and a single dust temperature T-d, and find that the dust temperature and emissivity index varies over the science demonstration field as <file name="mnr_17971_mu1.gif" type="gif"/> and 1 < beta < 4. The latter values are somewhat higher than the range of beta often quoted in the literature (1 < beta < 2). We estimate the mean values of these parameters to be T-d = 19.0 +/- 2.4 K and beta = 1.4 +/- 0.4. In regions of bright cirrus emission, we find that the dust has similar temperatures with <file name="mnr_17971_mu2.gif" type="gif"/>, and similar values of beta, ranging from 1.4 +/- 0.5 to 1.9 +/- 0.5. We show that T-d and beta associated with diffuse cirrus emission are anti-correlated and can be described by the relationship: beta(T-d) = NT alpha(d) with [N = 116 +/- 38, alpha = -1.4 +/- 0.1]. The strong correlation found in this analysis is not just limited to high-density clumps of cirrus emission as seen in previous studies, but is also seen in diffuse cirrus in low-density regions. To provide an independent measure of T-d and beta, we obtain the angular power spectrum of the cirrus emission in the IRAS and SPIRE maps, which is consistent with a power spectrum of the form P(k) = P-0(k/k(0))gamma, where gamma = 2.6 +/- 0.2 for scales of 50-200 arcmin in the SPIRE maps. The cirrus rms fluctuation amplitude at angular scales of 100 arcmin is consistent with a modified blackbody SED with <file name="mnr_17971_mu3.gif" type="gif"/> and beta = 1.3 +/- 0.2, in agreement with the values obtained above.

引用

页码：1151 / 1161

页数：11

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