Fourier-space combination of Planck and Herschel images

被引：10

作者：

Abreu-Vicente, J. ^{[1
,6
]}

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

Henning, Th. ^{[1
]}

Keto, E. ^{[3
]}

Ballesteros-Paredes, J. ^{[4
,5
]}

Robitaille, T. ^{[1
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] Univ Concepcion, Dept Astron, Av Esteban Iturra S-N,Distrito Univ,160-C, Concepcion, Chile

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[4] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Campus Morelia Apartado Postal 3-72, Morelia 58090, Michoacan, Mexico

[5] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany

[6] Heidelberg Univ, Int Max Planck Res Sch, Heidelberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 604卷

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

submillimeter: ISM; infrared: ISM; techniques: image processing; ISM: structure; DUST OPTICAL-DEPTH; INFRARED-EMISSION; SPIRE; MAPS; DISTRIBUTIONS; EVOLUTION; SPITZER; CLOUDS; PACS;

D O I：

10.1051/0004-6361/201628891

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Herschel has revolutionized our ability to measure column densities (N-H) and temperatures (T) of molecular clouds thanks to its far infrared multiwavelength coverage. However, the lack of a well defined background intensity level in the Herschel data limits the accuracy of the N-H and T maps. Aims. We aim to provide a method that corrects the missing Herschel background intensity levels using the Planck model for foreground Galactic thermal dust emission. For the Herschel/PACS data, both the constant-offset as well as the spatial dependence of the missing background must be addressed. For the Herschel/SPIRE data, the constant-offset correction has already been applied to the archival data so we are primarily concerned with the spatial dependence, which is most important at 250 mu m. Methods. We present a Fourier method that combines the publicly available Planck model on large angular scales with the Herschel images on smaller angular scales. Results. We have applied our method to two regions spanning a range of Galactic environments: Perseus and the Galactic plane region around l = 11 deg (HiGal-11). We post-processed the combined dust continuum emission images to generate column density and temperature maps. We compared these to previously adopted constant-offset corrections. We find significant differences (greater than or similar to 20%) over significant (similar to 15%) areas of the maps, at low column densities (N-H less than or similar to 10(22) cm(-2)) and relatively high temperatures (T greater than or similar to 20 K). We have also applied our method to synthetic observations of a simulated molecular cloud to validate our method. Conclusions. Our method successfully corrects the Herschel images, including both the constant-offset intensity level and the scale-dependent background variations measured by Planck. Our method improves the previous constant-offset corrections, which did not account for variations in the background emission levels.

引用

页数：13

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