adsabs/AstroCLIMB huggingface dataset:
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Herschel-derived column density map of the Aquila molecular clouds from the Herschel Gould Belt Survey (André et al. 2010). A gray dashed line separates Aquila-North and Aquila-South. The spatial coverage of the IRAC, MIPS, and PACS 100 μm maps are shown by yellow, green, and orange contours, respectively. PACS 70 and 160 μm, and SPIRE 250, 350, and 500 μm maps cover the entire displayed region. The major star-forming regions in Aquila-North and Aquila-South are labeled.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Herschel-derived dust temperature map of the Aquila molecular clouds from the Herschel Gould Belt Survey (André et al. 2010). A gray dashed line separates Aquila-North and Aquila-South. The major star-forming regions in Aquila-North and Aquila-South are labeled.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Panels (a), (b), and (c) show the scatter plots of L bol, N(H2), and R, respectively for the high-confidence protostars, pre-MS stars with disks, and galaxies. Panel (d) is a repetition of panel (c) but with a marker size proportional to R and colors that depend on the T bol. In all panels, the horizontal and vertical lines correspond to the 75th percentile of L bol, N(H2), and R for the high-confidence galaxies in our sample.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: An example of compact source identification in SPIRE and SCUBA-2 maps. In each panel, the left image shows the source, and green circles show aperture and annulus sizes for 250, 350, 500, and 850 μm maps, respectively. Dashed green circles represent the annulus over which we estimate the background flux. The right image shows the radial profile plot for the image on the left. Vertical lines show aperture and annulus sizes that correspond to the left image. The sky value is shown by a gray dashed horizontal line. The magenta lines shows the interpolated radial profile. The source is classified as a compact source at 250, 350, and 500 μm but not at 850 μm according to the MAD analysis.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Best-fit results with extragalactic templates overplotted to the SEDs of three galaxies in Aquila. The template number and R value for the best-fitting model are noted. Model template numbers from #1 to #8 refer to galaxies from actively star-forming to AGN-dominated (see Kirkpatrick et al. 2015). The sources are #2067206, #192641, and #36616 from left to right (see Table 10). These galaxies are identified using the template fitting criteria in Step 2.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: A few examples of SEDs of protostars in Aquila regions that are identified using Equation (7) defined in Section 4.1.4. The sources are eHOPS-aql-67 (Class 0), eHOPS-aql-48 (Class I), and eHOPS-aql-2 (flat-spectrum), respectively, from left to right. These protostars are identified as part of Step 3.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Three examples of reddened pre-MS stars with disks in Aquila regions that are identified using criteria defined in Section 4.1.4. The sources are #280461, #61202, and #120110 from left and right (see Table 9). These are identified as part of Step 3.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: A few examples of SEDs of pre-MS stars with disks in Aquila that are identified using Equation (8) defined in Section 4.1.4. The sources are #122731, #1225768, and #106653 from left to right (see Table 9). These pre-MS stars with disks are identified as part of Step 3.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: SEDs for some star-forming galaxies with prominent PAH emission at ∼8 μm that are found using the Spitzer/IRAC color criterion in Stutz et al. (2013). The sources are #1288709, #1186350, and #1218688 from left to right (see Table 10). These are identified as a part of Step 2.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Three examples of high-confidence protostars that are selected using the requirements in Section 4.1.2. The protostars are eHOPS-aql-18, eHOPS-aql-35, and eHOPS-aql-74 from left to right. All sources exhibit prominent silicate absorption features at 10 and 20 μm, and rising SEDs in the ∼ 1–100 μm wavelength range.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Examples of high-confidence pre-MS stars with disks that are selected using the requirements in Section 4.1.2. The sources are #30016, #50600, and #88493 from left to right (see Table 9).
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Variation of ν F  ν (70) with ν F  ν (70)/ν F  ν (24). (b) Variation of ν F  ν (100) with ν F  ν (100)/ν F  ν (24). Orange squares denote newly identified galaxies, maroon diamonds denote newly identified protostars, and blue triangles are newly identified pre-MS stars with disks.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Plot showing α 5.8,8.0 vs. α 3.6,4.5 and (b) α 3.6,100 vs. α 3.6,4.5. Maroon diamonds and blue triangles denote reclassified protostars and pre-MS stars with disks, respectively. The horizontal and vertical dashed lines in panel (a) denote α 5.8,8.0 = 2 and α 3.6,4.5 = 0.5, respectively. In the legend, CP stands for CPs.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Three examples of SEDs of CPs in Aquila identified using the criteria defined in Section 4.1.4. The SED in the left panel is a galaxy confirmed from near-IR morphology that escaped our selection criteria (#78912 in Table 10). The middle and right panels show SEDs of two protostars, eHOPS-aql-76, and eHOPS-aql-141, respectively. These are identified as part of Step 3.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Protostars (yellow circles) and pre-MS stars with disks (cyan circles) overplotted on the column density map of Aquila star-forming clouds. The central Galactic latitude line (b = 0°) is shown for reference, and blue dashed lines show the surveyed regions. The protostars are mostly concentrated toward the dense regions of the cloud.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Distribution of projected column densities for protostars, pre-MS stars with disks, and galaxies in Aquila. Galaxies are mostly concentrated in lower N(H2) and protostars in higher N(H2) regions, respectively. (b) Variation of L bol with N(H2) for the same sources as in panel (a). Color labels in panel (b) are the same as in panel (a). In addition to being found in lower-density regions, galaxies also have lower L bol at the adopted distance of Aquila.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Similar to Figure 17 but galaxies are overplotted on the column density map. Unlike protostars, galaxies are mostly found in less-dense regions.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Examples of SEDs of pre-MS stars with disks that show steeply falling mid-to-far-IR emission but are not identified on the basis of the mid-IR photometry due to missing photometry. The sources are #290129, #409790, and #1303802 from left to right (see Table 9). These are identified using the completeness limits in Step 5.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Bolometric temperatures (T bol) for SEDs of sources vs. Herschel-derived dust temperature (T dust) at their position (see Figure 46). This diagram is used to identify starless cores in our sample. Sources in empty black circles are starless cores. This analysis is part of Step 5.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Histogram of the model-derived envelope reference density (ρ 1000) from the best fits of protostars in the eHOPS sample for Aquila. (b) Histogram of ρ 1000 separated by different SED classes. Class 0 protostars have the highest ρ 1000. A-D tests show significant differences in the distribution of ρ 1000 between Class 0 and the remaining classes, but no significant difference between Class I and flat-spectrum sources.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Histogram of the model-derived foreground extinction (A  V ) for the best fits of protostars in the eHOPS sample for Aquila. (b) Histogram of A  V  separated by different SED classes. The A-D test shows a significant difference in the distribution of Class 0 and flat-spectrum sources.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Variation of the best-fit envelope reference density (ρ 1000) with inclination angle (i) for different SED classes. The size of markers corresponds to the number of protostars with the same pair of (ρ 1000, i). The sizes that correspond to different numbers of protostars are shown in the lower region of the first panel. We find a majority of Class 0 protostars to be concentrated at intermediate to high inclination angles, whereas Class I protostars and flat-spectrum protostars are more uniformly distributed.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Foreground extinction values (A  V ) from the best-fit models vs. the maximum A  V  value determined from column density maps of Aquila. The dashed line indicates where the two A  V  values are equal. The model-derived A  V  is typically less than the projected column density at the position of protostars, confirming that the protostars are embedded in the clouds rather than in the background.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Histogram of the inclination angles (i) for the best fits of protostars in the eHOPS sample for Aquila, shown for different SED classes.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Variation of the best-fit envelope reference density ρ 1000 with foreground extinction A  V  for different SED classes.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Histogram of the best-fit inclination angles of the Aquila protostars. The gray dashed histogram shows the distribution of uniformly (randomly) distributed inclination angles. The inclination angles for the protostars in Aquila are not distributed randomly but peaked at ∼63°.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Histogram of ﹩{R}_{\min }﹩ values for the best fits of protostars in the eHOPS sample for Aquila, shown separately for the different evolutionary SED classes. Ninety-five percent of Class 0, 98% of Class I, and all flat-spectrum sources have reasonably good fits with ﹩{R}_{\min }\lt 5﹩ and ≥3 data points in their SEDs.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Histogram of ﹩{R}_{\min }﹩ values for the best fits of protostars in the eHOPS sample for Aquila. About 97% of the SEDs are well constrained with ≥3 data points in their SEDs and ﹩{R}_{\min }\lt 5﹩.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Variation of ν F  ν (70) with ν F  ν (70)/ν F  ν (24). (b) Variation of ν F  ν (100) with ν F  ν (100)/ν F  ν (24). In both panels, different colored symbols show different evolutionary classes as noted in the legend. Black open boxes show the extremely red protostars that are detected in Sections 4.1.5 and 4.1.6. Open circles denote that the protostars are not detected at 24 μm so the corresponding completeness limit is used as an upper limit flux. Filled circles denote the protostars where 24 μm photometry is available. The red vertical dashed lines in both panels mark the criteria that we use to find PBRSs; ν F  ν (70)/ν F  ν (24) = 101.65 for panel (a) (from Stutz et al. 2013) and ν F  ν (100)/ν F  ν (24) = 101.85 for panel (b) (see Section 4.1.5).
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: Variation in the ratio of total luminosity to bolometric luminosity with inclination angle (left panel) and foreground extinction (middle panel) for the eHOPS protostars in Aquila. The right panel is the same as the middle panel but in linear units of the foreground extinction. Blue stars mark the median L tot/L bol ratio for specific bins of i and A  V , and the horizontal lines overlaid on the stars show the range of the A  V  bin. As the inclination angle of protostars increases (toward edge-on configuration), the ratio L tot/L bol also increases. A similar trend is seen as an effect of foreground extinction.
Paper: Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds 
Authors: Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman, John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj, Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri
Figure caption: (a) Histogram of the model-derived total luminosities (L tot) from the best fits of protostars in the eHOPS sample for Aquila. We find that L tot peaks at ∼5.4 L ☉. (b) The same as panel (a) but for different evolutionary classes. The A-D test shows no significant difference in the distribution of L tot for different SED classes.