\ Project: extension of HOPS out to 500 ParSecs (eHOPS) \ PI: S. T. Megeath \ Citation: Pokhrel et al. (2023b) \ Table info: Photometry in the 1-850 micron wavelengths for candidate protostars (CPs) \ Index \ ___ Arbitrary running index \ ra (degrees) \ ___ Right Ascension (J2000) \ dec (degrees) \ ___ Declination (J2000) \ *_flux (Jy) \ ___ flux density \ e_*_flux (Jy) \ ___ flux density uncertainty \ c_*_flux \ ___ completeness limit on the flux density (underestimated if the source is not detected due to saturation) \ ___ if "U", flux density is used as an upper limit \ s_*_flux \ ___ sky limit (underestimated if the source is not detected due to saturation) \ ___ if "U", flux density is used as an upper limit \ photometric bands: \ 2MASS: J (1.25 micron), H (1.65 micron), Ks (2.17 micron) \ Spitzer/IRAC: I1 (3.6 micron), I2 (4.5 micron), I3 (5.8 micron), I4 (8.0 micron) \ Spitzer/MIPS: M1 (24 micron) \ WISE: W1 (3.4 micron), W2 (4.6 micron), W3 (12 micron), W4 (22 micron) \ Herschel/PACS: P1 (70 micron), P2 (100 micron), P3 (160 micron) \ Herschel/SPIRE: SP1 (250 micron), SP2 (350 micron), SP3 (500 micron) \ JCMT/SCUBA2: SC (850 micron) \ Comments: Reason for classifying the source as a CP \fixlen = T | Index| ra| dec|J_flux|e_J_flux|H_flux|e_H_flux|Ks_flux|e_Ks_flux|I1_flux|e_I1_flux|c_I1_flux|I2_flux|e_I2_flux|c_I2_flux|I3_flux|e_I3_flux|c_I3_flux|I4_flux|e_I4_flux|c_I4_flux|M1_flux|e_M1_flux|c_M1_flux|W1_flux|e_W1_flux|W2_flux|e_W2_flux|W3_flux|e_W3_flux|W4_flux|e_W4_flux|P1_flux|e_P1_flux|s_P1_flux|P2_flux|e_P2_flux|s_P2_flux|P3_flux|e_P3_flux|s_P3_flux|SP1_flux|e_SP1_flux|s_SP1_flux|SP2_flux|e_SP2_flux|s_SP2_flux|SP3_flux|e_SP3_flux|s_SP3_flux|SC_flux|e_SC_flux|s_SC_flux| Comments| | long| double| double| long| long| long| long| long| long| double| long| double| double| long| double| long| long| double| double| double| double| double| double| double| long| long| long| long| long| long| long| long| long| long| double| double| double| double| double| double| double| double| double| char| double| double| char| double| double| char| long| long| long| char| | | degrees| degrees| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| mJy| | | null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| null| 20804 285.98384 -37.23322 null null null null null null null null null null null 0.1 null null 0.2 null null 0.2 null null 0.5 null null null null null null null null null null 17.1 null null 3.6 58.4 7.6 8.6 3979.3 5.4 U 5306.7 8.9 U 6056.7 13.9 U null null null Step 5--- Using completeness limits for one or more IRAC photometry 42127 285.29163 -36.94317 null null null null null null 0.1 null 0.2 0.1 null 0.3 null null 2.8 0.2 null 0.8 null null 32.0 null null null null null null null null null null 15.4 92.6 5.1 2.1 null null 3.9 3191.7 6.6 U 3262.7 6.9 U 3248.6 9.8 U null null null Step 5--- Using completeness limits for one or more IRAC photometry 42646 285.43042 -36.98678 null null null null null null 0.1 null 0.3 0.1 null 0.2 null null 3.6 0.6 0.1 1.0 null null 236.4 null null null null null null null null null null 16.7 84.7 4.7 2.1 null null 4.1 6022.6 16.1 U 6657.0 28.5 U 8097.7 49.2 U null null null Step 5--- Using completeness limits for one or more IRAC photometry 101233 285.52355 -36.91051 null null null null null null null null 0.6 null null 1.9 null null 2.3 null null 1.9 6.5 0.4 17.3 null null null null null null null null null null 16.7 163.6 8.4 2.0 null null 3.8 4227.7 6.2 U 4890.8 7.7 U 4693.5 7.6 U null null null Step 5--- Using completeness limits for one or more Spitzer or Herschel/PACS photometry