Edge-on protostars are valuable for understanding the disk and envelope properties of embedded young stellar objects , since the disk , envelope , and envelope cavities are all distinctly visible in resolved images and well constrained in modeling .
Comparing 2MASS , WISE , Spitzer , Herschel , APEX , and IRAM photometry and limits from 1.25 to 1200 µm , Spitzer spectroscopy from 5 to 40 µm , and high-resolution Hubble imaging at 1.60 and 2.05 µm to radiative transfer modeling , we determine envelope and disk properties for the Class I protostar HOPS 136 , an edge-on source in Orion ’ s Lynds 1641 region .
The source has a bolometric luminosity of 0.8 L _ { \sun } , a bolometric temperature of 170 K , and a ratio of submillimeter to bolometric luminosity of 0.8 % .
Via modeling , we find a total luminosity of 4.7 L _ { \sun } ( larger than the observed luminosity due to extinction by the disk ) , an envelope mass of 0.06 M _ { \sun } , and a disk radius and mass of 450 AU and 0.002 M _ { \sun } .
The stellar mass is highly uncertain but is estimated to fall between 0.4 and 0.5 M _ { \sun } .
To reproduce the flux and wavelength of the near-infrared scattered-light peak in the spectral energy distribution , we require 5.4 \times 10 ^ { -5 } ~ { } M _ { \sun } of gas and dust in each cavity .
The disk has a large radius and a mass typical of more evolved T Tauri stars in spite of the significant remaining envelope .
HOPS 136 appears to be a key link between the protostellar and optically revealed stages of star formation .