\ Project: extension of HOPS out to 500 ParSecs (eHOPS) \ PI: S. T. Megeath \ Citation: Pokhrel et al. (2023) \ 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| char| char| char| char| char| char| char| char| char| char| char| double| char| char| char| char| char| double| char| char| double| char| char| char| char| char| char| char| char| char| char| double| double| double| double| char| char| double| double| double| char| double| double| char| double| double| char| char| char| char| 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| | 133408 277.41307 1.20937 --- --- --- --- --- --- --- --- 0.2 --- --- 0.2 --- --- 0.3 0.2 --- 0.2 --- --- 1.2 --- --- --- --- --- --- --- --- --- --- 16.9 150.6 9.8 6.3 492.7 26.2 11.1 4857.2 10.0 U 5184.0 10.6 U 5149.2 12.6 U --- --- --- Step 5--- Extended resolved emission at $\ge$100 $\micron$ 136261 277.48827 1.24477 5.6 0.5 --- --- --- --- --- --- 54.6 --- --- 35.0 --- --- 34.0 --- --- 370.3 --- --- 4320.4 --- --- --- --- --- --- --- --- 11929.3 605.4 103.8 9665.6 483.6 18.9 --- --- 44.8 35817.0 121.3 U 34353.8 162.5 U 33074.0 170.1 U 734.2 48.3 U Step 5--- Using completeness limits for one or more Spitzer or Herschel/PACS photometry 136301 277.5818 1.09293 --- --- --- --- --- --- 0.3 --- 0.4 0.3 --- 1.3 0.2 --- 0.3 0.3 --- 0.9 9.0 0.2 15.4 --- --- --- --- --- --- --- --- --- --- 17.7 57.3 6.8 6.1 --- --- 11.0 206.1 17.1 110.3 59.1 14.9 172.9 2908.8 5.3 U --- --- --- Step 3--- [3.6]-[4.5] $<$ 0.65, $\alpha_{4.5,24} > 0.3$ 647743 277.15377 -3.59109 --- --- --- --- --- --- 0.1 --- 0.8 0.1 --- 0.3 --- --- 0.3 --- --- 0.2 2.5 0.1 2.9 --- --- --- --- --- --- --- --- --- --- 19.9 106.7 7.1 4.8 --- --- 10.5 231.0 34.6 205.3 6135.2 5.3 U 5870.4 6.4 U --- --- --- Step 3--- [3.6]-[4.5] $<$ 0.65, $\alpha_{4.5,24} > 0.3$ 855983 277.42673 -3.08261 --- --- --- --- --- --- --- --- 0.9 --- --- 0.5 --- --- 0.4 0.4 --- 0.6 --- --- 1.4 --- --- --- --- --- --- --- --- --- --- 16.5 93.0 7.0 5.2 --- --- 10.6 4411.2 4.0 U 4460.1 4.7 U 4140.2 5.8 U --- --- --- Step 5--- Using completeness limits for one or more Spitzer or Herschel/PACS photometry 1080177 277.75456 -2.59728 --- --- --- --- --- --- 0.3 --- 0.7 0.2 --- 0.4 --- --- 0.5 1.2 0.1 0.5 3.5 0.2 3.1 --- --- --- --- --- --- --- --- --- --- 18.4 140.5 9.3 6.1 279.7 16.5 10.6 6075.1 4.7 U 5947.1 4.6 U 5524.9 6.0 U --- --- --- Step 3--- [3.6]-[4.5] $<$ 0.65, $\alpha_{4.5,24} > 0.3$ 1091248 278.48399 -2.64829 --- --- --- --- 0.7 0.1 --- --- --- 0.5 --- 0.5 --- --- --- 1.1 --- 1.1 4.6 0.2 1.4 0.6 --- 0.4 --- 2.4 0.2 4.2 1.1 --- --- 16.6 102.6 7.7 5.8 --- --- 12.5 4448.2 5.0 U 4388.5 5.2 U 4037.0 6.8 U --- --- --- Step 3--- [3.6]-[4.5] $<$ 0.65, $\alpha_{4.5,24} > 0.3$ 1234796 278.26457 -2.14512 --- --- 1.9 0.1 3.1 0.2 7.4 0.1 3.5 8.6 0.1 1.7 18.9 0.3 2.9 48.3 0.6 6.3 603.2 5.7 5.4 7.2 0.2 9.7 0.2 69.4 1.0 640.9 10.0 --- --- 20.4 170.5 10.3 5.7 --- --- 11.2 4061.5 4.0 U 3926.3 4.1 U 3613.6 5.4 U --- --- --- Step 3--- [3.6]-[4.5] $<$ 0.65, $\alpha_{4.5,24} > 0.3$ 1301597 278.01351 -1.84771 --- --- --- --- --- --- --- --- 0.6 0.1 --- 0.6 --- --- 0.6 0.2 --- 0.3 --- --- 2.1 --- --- --- --- --- --- --- --- --- --- 17.7 78.5 7.2 6.0 --- --- 10.8 8406.4 5.6 U 8880.0 6.4 U 8674.2 9.0 U --- --- --- Step 5--- Using completeness limits for one or more IRAC photometry 2060574 277.11986 -3.78166 --- --- --- --- --- --- --- --- 79.2 --- --- 56.8 --- --- 24.3 --- --- 169.9 --- --- 16.1 --- --- --- --- --- --- --- --- --- --- 16.2 161.2 9.6 5.3 200.5 13.5 11.1 7629.2 6.6 U 8312.4 10.7 U 8178.2 13.2 U --- --- --- Step 5--- Extended resolved emission at $\ge$100 $\micron$ 2066950 277.25521 0.5029 --- --- --- --- --- --- --- --- 1.7 --- --- 1.1 --- --- 6.3 --- --- 1.8 --- --- 180.1 --- --- --- --- --- --- --- --- --- --- 16.4 751.2 38.0 6.1 3457.9 174.3 16.7 12397.6 44.4 U 14188.8 45.6 U 14946.3 37.7 U --- --- --- Step 5--- Extended resolved emission at $\ge$100 $\micron$ 2067887 277.50791 1.25285 --- --- --- --- --- --- --- --- 0.2 --- --- 8.3 --- --- 0.4 --- --- 17.4 --- --- 48.8 --- --- --- --- --- --- --- --- --- --- 17.6 773.8 39.2 6.1 3490.6 179.5 18.4 17476.7 43.4 U 19395.8 52.2 U 19391.3 59.0 U 323.6 25.0 4.7 Step 5--- Extended resolved emission at $\ge$100 $\micron$