CEA
Herschel Gould Belt Survey Archive
Herschel Gould Belt Survey Archive

Spatial distribution of Aquila prestellar dense cores (blue triangles) over (the curvelet component of) the Herschel column density map.

Herschel provides a unique opportunity to study the earliest stages of star formation. What is the origin of the stellar initial mass function (IMF) ? This issue is central in local star formation research and for understanding whether the IMF is truly universal or is likely to depend on metallicity, pressure, or temperature. As prestellar cores and young (Class 0) protostars emit the bulk of their luminosity at ~80-400 microns, the Herschel imaging instruments SPIRE and PACS are ideal for taking a census of such objects down to ~0.01-0.1 Msun in the nearby (0.5 kpc) molecular cloud complexes. We propose an extensive imaging survey of the densest portions of the Gould Belt with SPIRE at 250-500 and PACS at 110-170 microns down to a 5-sigma column sensitivity NH2~1021 cm^-2 or Av~1. Our goal is to make a complete, homogeneous mapping of the Av>3 regions with SPIRE and of the Av>6 regions with PACS, and representative areas at Av~1-3 levels with both instruments. The survey sensitivity is well matched to the expected cirrus confusion limit, so we should detect structures throughout the maps. The target clouds span a range of physical conditions, from active, cluster-forming complexes to quiescent regions with lower star formation activity. We should detect hundreds Class 0 protostars and thousands prestellar condensations in the entire ~145 deg^2 SPIRE survey, i.e. ~10 times more cold objects than already identified from the ground. These numbers should allow us to derive an accurate prestellar core mass function. The temperature and density structures of the nearest ( 0.2 kpc) cores will be resolved, revealing the initial conditions for individual protostellar collapse. The large spatial dynamic range of the proposed survey will probe the link between diffuse cirrus-like structures and compact self-gravitating cores. Our main scientific goal is to elucidate the physical mechanisms for the formation of prestellar cores out of the diffuse medium, crucial for understanding the origin of stellar masses.

ACKNOWLEDGEMENTS:

Every work using Herschel Gould Belt survey data should include the following acknowledgement text:

This research has made use of data from the Herschel Gould Belt survey (HGBS) project (http://gouldbelt-herschel.cea.fr). The HGBS is a Herschel Key Programme jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium (CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg), and scientists of the Herschel Science Center (HSC).

and cite the introductory paper of the Herschel Gould Belt survey by André et al. (2010, A&A, 518, L102).

 
Regions

PACS  70 µm images

PACS 100µm images PACS 160µm images SPIRE
250µm images
SPIRE
350µm images
SPIRE
500µm images

Catalogs of dense cores

Column density and temperature maps References
Acknowledgements
Aquila aquilaM2-070   aquilaM2-160 aquilaM2-250 aquilaM2-350 aquilaM2-500

HGBS_aquilaM2_observed_core_catalog.txt

HGBS_aquilaM2_derived_core_catalog.txt

HGBS_aquilaM2_core_blowups.pdf

HGBS_aquilaM2_core_SEDs.pdf

HGBS_aquilaM2_column_density_map.fits.gz

HGBS_aquilaM2_dust_temperature_map.fits.gz

Könyves et al. 2010

Bontemps et al. 2010

André et al. 2010

Könyves et al. 2015

Cepheus            

Expected availability: June 2018

Contact: James Di Francesco

HGBS_cep1157_column_density_map.fits

HGBS_cep1157_dust_temperature_map.fits.gz

HGBS_cep1172_column_density_map.fits

HGBS_cep1172_dust_temperature_map.fits.gz

HGBS_cep1228_column_density_map.fits

HGBS_cep1228_dust_temperature_map.fits.gz

HGBS_cep1241_column_density_map.fits

HGBS_cep1241_dust_temperature_map.fits.gz

HGBS_cep1251_column_density_map.fits

HGBS_cep1251_dust_temperature_map.fits.gz

Di Francesco et al., in prep.
Chamaleon chamI-070   chamI-160 chamI-250 chamI-350 chamI-500  

chamI-coldens

chamI-Tdust

chamII-coldens

chamII-Tdust

chamIII-coldens

chamIII-Tdust

Winston et al. 2012

Kospal et al. 2012

Alves de Oliveira al. 2014

Coalsack               Expected: September 2017  
Corona Australis craNS-070   craNS-160 craNS-250 craNS-350 craNS-500

HGBS_craNS_observed_core_catalog.txt

HGBS_craNS_derived_core_catalog.txt

HGBS_craNS_core_blowups.pdf

HGBS_craNS_core_SEDs.pdf

 

HGBS_craNS_column_density_map.fits.gz

HGBS_craNS_dust_temperature_map.fits.gz

Bresnahan et al. 2018

Sicilia-Aguilar et al. 2013

IC5146 ic5146-070   ic5146-160 ic5146-250 ic5146-350 ic5146-500  

HGBS_ic5146_column_density_map.fits.gz

HGBS_ic5146_dust_temperature_map.fits.gz

Arzoumanian et al. 2011
Lupus lupusI-070   lupusI-160 lupusI-250 lupusI-350 lupusI-500

HGBS_lupI_observed_core_catalog.txt

HGBS_lupI_derived_core_catalog.txt

HGBS_lupI_core_blowups_seds.pdf

Contact: Milena Benedettini

HGBS_lupI_column_density_map.fits.gz

HGBS_lupI_dust_temperature_map.fits.gz

HGBS_lupIII_column_density_map.fits.gz

HGBS_lupIII_dust_temperature_map.fits.gz

HGBS_lupIV_column_density_map.fits.gz

HGBS_lupIV_dust_temperature_map.fits.gz

Rygl et al. 2013

Benedettini et al. 2018

Musca              

HGBS_musca_column_density_map.fits.gz

HGBS_musca_dust_temperature_map.fits.gz

Cox et al. 2016

Ophiuchus

& L1689B

L1689B-070   L1689B-160 L1689B-250 L1689B-350 L1689B-500

Expected availability: November 2017

Contact: Bilal Ladjelate

HGBS_oph_l1688_column_density_map.fits.gz

HGBS_oph-L1688_dust_temperature_map.fits.gz

L1689B-coldens

L1689B-Tdust

Ladjelate et al. 2018

Roy et al. 2014

Orion A

orionA-C-070

orionA-S-070

 

orionA-C-160

orionA-S-160

orionA-C-250

orionA-S-250

orionA-C-350

orionA-S-350

orionA-C-500

orionA-S-500

Expected availability (Orion A S): End of 2017

Contact: Danae Polychroni

Expected: September 2017

Roy et al. 2013

Polychroni et al. 2013

Orion B orionB-S-070   orionB-S-160 orionB-250 orionB-350 orionB-500

Expected availability: October 2017

Contact: Vera Könyves

HGBS_orionB_column_density_map.fits.gz

HGBS_orionB_dust_temperature_map.fits.gz

Schneider  et al. 2013

Könyves et al. 2018

Perseus perseus-070   perseus-160 perseus-250 perseus-350 perseus-500

Expected availability: March 2018

Contact: Stefano Pezzuto

HGBS_perseus_column_density_map.fits.gz

HGBS_perseus_dust_temperature_map.fits.gz

Pezzuto et al. 2012

Sadavoy et al. 2012

Sadavoy et al. 2014

Pipe nebula

and B68

pipe-070

b68-070

 

pipe-160

b68-160

pipe-250

b68-250

pipe-350

b68-350

pipe-500

b68-500

Expected availability: January 2018

Contact: Arabindo Roy

HGBS_pipe_column_density_map.fits.gz

HGBS_pipe_dust_temperature_map.fits.gz

b68-coldens

b68-Tdust

Peretto et al. 2012

Roy et al. 2014

Roy et al. 2018

Polaris polaris-070 polaris-100 polaris-160 polaris-250 polaris-350 polaris-500  

HGBS_polaris_column_density_map.fits.gz

HGBS_polaris_dust_temperature_map.fits.gz

 

Menshchikov et al. 2010

Miville-Deschênes et al. 2010

Ward-Thompson et al. 2010

André et al. 2010

Taurus

tauL1495-070

  tauL1495-160 tauL1495-250 tauL1495-350 tauL1495-500

HGBS_taurusL1495_observed_core_catalog.txt

HGBS_taurusL1495_derived_core_catalog.txt

HGBS_taurusL1495_core_blowups_and_SEDs.pdf

 

HGBS_taurus_L1495_column_density_map.fits.gz

HGBS_taurus_L1495_dust_temperature_map.fits.gz

 

Palmeirim et al. 2013

Kirk et al. 2013

Marsh et al. 2014

Marsh et al. 2016

Serpens            

Expected availability: March 2018

Contact: Stefano Pezzuto

HGBS_serpens_column_density_map.fits.gz

HGBS_serpens_dust_temperature_map.fits.gz

 

 

 

Last update : 10/01 2018 (66)

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