eHOPS SED Data Catalog Definitions

Overview

The Extension of HOPS Out to 500 ParSecs (eHOPS) project used archival data to survey all the major star forming molecular clouds within 500 pc of the Sun, except Orion (which was surveyed by HOPS). For every source detected in the Herschel/PACS bands, the eHOPS SED catalogs contain 1-850 micron SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. eHOPS compares the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities, and envelope masses of the protostars.

To query for all sources in a molecular cloud, do an All Sky Search with an SQL Constraint (bottom of search page) on eHOPS_ID, for example "eHOPS_ID like ' eHOPS-oph%'" for all sources in Ophiuchus. Or simply do an All Sky Search and filter the eHOPS_ID column of the results table. The ID strings for each cloud are:

Cloud NameCloud ID
Aquilaaql
Aurigaaur
Cepheuscep
Chamaeleoncha
CrAcra
Lupuslup
Muscamus
Ophiuchusoph
Perseusper
Pipepipe

If you use eHOPS Aquila data please cite Pokhrel et al. 2023.

Name Intype Units Description
eHOPS_ID char eHOPS ID
ra double degrees Right Ascension (J2000)
dec double degrees Declination (J2000)
J_flux double mJy 2MASS J (1.25 micron) flux density
e_J_flux double mJy 2MASS J (1.25 micron) flux density uncertainty
H_flux double mJy 2MASS H (1.65 micron) flux density
e_H_flux double mJy 2MASS H (1.65 micron) flux density uncertainty
Ks_flux double mJy 2MASS Ks (2.17 micron) flux density
e_Ks_flux double mJy 2MASS Ks (2.17 micron) flux density uncertainty
I1_flux double mJy Spitzer/IRAC I1 (3.6 micron) flux density
e_I1_flux double mJy Spitzer/IRAC I1 (3.6 micron) flux density uncertainty
c_I1_flux double mJy Spitzer/IRAC I1 (3.6 micron) flux density completeness limit
I2_flux double mJy Spitzer/IRAC I2 (4.5 micron) flux density
e_I2_flux double mJy Spitzer/IRAC I2 (4.5 micron) flux density uncertainty
c_I2_flux double mJy Spitzer/IRAC I2 (4.5 micron) flux density completeness limit
I3_flux double mJy Spitzer/IRAC I3 (5.8 micron) flux density
e_I3_flux double mJy Spitzer/IRAC I3 (5.8 micron) flux density uncertainty
c_I3_flux double mJy Spitzer/IRAC I3 (5.8 micron) flux density completeness limit
I4_flux double mJy Spitzer/IRAC I4 (8 micron) flux density
e_I4_flux double mJy Spitzer/IRAC I4 (8 micron) flux density uncertainty
c_I4_flux double mJy Spitzer/IRAC I4 (8 micron) flux density completeness limit
M1_flux double mJy Spitzer/MIPS M1 (24 micron) flux density
e_M1_flux double mJy Spitzer/MIPS M1 (24 micron) flux density uncertainty
c_M1_flux double mJy Spitzer/MIPS M1 (24 micron) flux density completeness limit
W1_flux double mJy WISE W1 (3.4 micron) flux density
e_W1_flux double mJy WISE W1 (3.4 micron) flux density uncertainty
W2_flux double mJy WISE W2 (4.6 micron) flux density
e_W2_flux double mJy WISE W2 (4.6 micron) flux density uncertainty
W3_flux double mJy WISE W3 (12 micron) flux density
e_W3_flux double mJy WISE W3 (12 micron) flux density uncertainty
W4_flux double mJy WISE W4 (22 micron) flux density
e_W4_flux double mJy WISE W4 (22 micron) flux density uncertainty
P1_flux double mJy Herschel/PACS P1 (70 micron) flux density
e_P1_flux double mJy Herschel/PACS P1 (70 micron) flux density uncertainty
s_P1_flux double mJy Herschel/PACS P1 (70 micron) flux density sky limit
P2_flux double mJy Herschel/PACS P2 (100 micron) flux density
e_P2_flux double mJy Herschel/PACS P2 (100 micron) flux density uncertainty
s_P2_flux double mJy Herschel/PACS P2 (100 micron) flux density sky limit
P3_flux double mJy Herschel/PACS P3 (160 micron) flux density
e_P3_flux double mJy Herschel/PACS P3 (160 micron) flux density uncertainty
s_P3_flux char mJy Herschel/PACS P3 (160 micron) flux density sky limit
SP1_flux double mJy Herschel/SPIRE SP1 (250 micron) flux density
e_SP1_flux double mJy Herschel/SPIRE SP1 (250 micron) flux density uncertainty
s_SP1_flux char mJy Herschel/SPIRE SP1 (250 micron) flux density sky limit
SP2_flux double mJy Herschel/SPIRE SP2 (350 micron) flux density
e_SP2_flux double mJy Herschel/SPIRE SP2 (350 micron) flux density uncertainty
s_SP2_flux char mJy Herschel/SPIRE SP2 (350 micron) flux density sky limit
SP3_flux double mJy Herschel/SPIRE SP3 (500 micron) flux density
e_SP3_flux double mJy Herschel/SPIRE SP3 (500 micron) flux density uncertainty
s_SP3_flux char mJy Herschel/SPIRE SP3 (500 micron) flux density sky limit
SC_flux double mJy JCMT/SCUBA2 SC (850 micron) flux density
e_SC_flux double mJy JCMT/SCUBA2 SC (850 micron) flux density uncertainty
s_SC_flux char mJy JCMT/SCUBA2 SC (850 micron) flux density sky limit
I0540_flux double mJy Spitzer IRS flux density at 5.4 micron
e_I0540_flux double mJy Spitzer IRS flux density uncertainty at 5.4 micron
I0645_flux double mJy Spitzer IRS flux density at 6.45 micron
e_I0645_flux double mJy Spitzer IRS flux density uncertainty at 6.45 micron
I0750_flux double mJy Spitzer IRS flux density at 7.5 micron
e_I0750_flux double mJy Spitzer IRS flux density uncertainty at 7.5 micron
I0810_flux double mJy Spitzer IRS flux density at 8.1 micron
e_I0810_flux double mJy Spitzer IRS flux density uncertainty at 8.1 micron
I0860_flux double mJy Spitzer IRS flux density at 8.6 micron
e_I0860_flux double mJy Spitzer IRS flux density uncertainty at 8.6 micron
I0920_flux double mJy Spitzer IRS flux density at 9.2 micron
e_I0920_flux double mJy Spitzer IRS flux density uncertainty at 9.2 micron
I0980_flux double mJy Spitzer IRS flux density at 9.8 micron
e_I0980_flux double mJy Spitzer IRS flux density uncertainty at 9.8 micron
I1050_flux double mJy Spitzer IRS flux density at 10.5 micron
e_I1050_flux double mJy Spitzer IRS flux density uncertainty at 10.5 micron
I1250_flux double mJy Spitzer IRS flux density at 12.5 micron
e_I1250_flux double mJy Spitzer IRS flux density uncertainty at 12.5 micron
I1400_flux double mJy Spitzer IRS flux density at 14 micron
e_I1400_flux double mJy Spitzer IRS flux density uncertainty at 14 micron
I1650_flux double mJy Spitzer IRS flux density at 16.5 micron
e_I1650_flux double mJy Spitzer IRS flux density uncertainty at 16.5 micron
I1900_flux double mJy Spitzer IRS flux density at 19 micron
e_I1900_flux double mJy Spitzer IRS flux density uncertainty at 19 micron
I2300_flux double mJy Spitzer IRS flux density at 23 micron
e_I2300_flux double mJy Spitzer IRS flux density uncertainty at 23 micron
I2700_flux double mJy Spitzer IRS flux density at 27 micron
e_I2700_flux double mJy Spitzer IRS flux density uncertainty at 27 micron
I3100_flux double mJy Spitzer IRS flux density at 31 micron
e_I3100_flux double mJy Spitzer IRS flux density uncertainty at 31 micron
I3500_flux double mJy Spitzer IRS flux density at 35 micron
e_I3500_flux double mJy Spitzer IRS flux density uncertainty at 35 micron
Comments char Reason for the protostar identification (see section 4 in Pokhrel et al. 2023)