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: Variation of bolometric luminosity (L bol) with total luminosity (L tot) for the eHOPS protostars in Aquila (left panel) and HOPS protostars in Orion (right panel). In both panels, the green dashed–dotted line shows the median value of L tot/L bol, the black dashed line is the region where L bol and L tot are the same, and the black dotted line represents L tot = 10 × L bol. The median L tot/L bol is similar in Aquila (2.4) and Orion (2.5).
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 mass within 2500au (M 2500) from the best fits of protostars in the eHOPS sample for Aquila. (b) Histogram of M 2500 separated by different SED classes. Class 0 protostars have the highest M 2500. A-D tests show significant differences in the distribution of M 2500 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: The cumulative distribution function (CDF) of L bol for protostars in Aquila and Orion molecular clouds is shown in panel (a). The CDF for L tot for the same clouds is shown in panel (b). The A-D test shows no significant difference in the distributions of L bol and L tot in Aquila and Orion for protostars with L bol > 0.1 L ☉.
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: The PLFs using L bol for the eHOPS-Aquila protostars (panel (a)), HOPS protostars (panel (b)), and HOPS protostars separately for Orion A and Orion B (panel (c)). The median, the first quartile (Q1), and the third quartile (Q3) values of the distribution are given and indicated by vertical lines. The A-D test shows that the PLFs for Aquila and Orion B are likely drawn from the same parent distribution, but that this is unlikely for the Aquila and Orion A PLFs.
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: The PLFs using L tot for the eHOPS-Aquila protostars (panel (a)), HOPS protostars (panel (b)), and HOPS protostars separately for Orion A and Orion B (panel (c)). The median, the first quartile (Q1), and the third quartile (Q3) values of the distribution are given and indicated by vertical lines. The A-D test indicates that we cannot rule out that they are drawn from the same parent population.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: (a) and (b) present the member and parallax distribution of 1179 OCs, respectively. The histograms of the age and Z of 1179 OCs are shown in (c) and (d), respectively.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: As same as Figure 1, but for Examples of class B.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: Examples of class A. From left-hand to right-hand, the subplots show the spatial distribution, proper-motion distribution, parallax statistics, parallax distribution, and CMD with best-fitting isochrone line, respectively. The color bars represent the cluster probability of the member stars.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: Schematic diagram of the results (i.e., NGC 188, NGC 1662, NGC 2682, and NGC 752) of matching with CG20.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: Distribution of the OC candidates. Matched known clusters (blue triangles), the Cantat-Gaudin et al. (2020; CG20) OCs (gray dots), and the new 1179 OCs (red dots) are given, respectively.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: Same as Figure 1 but for Examples of class C.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: An example of high-Galactic-latitude OCs.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: RV dispersion distribution diagram (a) and mean distribution diagram (b) of 1179 OCs compared with H22 and CG22, respectively. RV standard deviation distribution diagram (c) and PMD diagram (d) of 1179 OCs compared with CG22 and CG20, respectively.
Paper: Blind Search of the Solar Neighborhood Galactic Disk within 5 kpc: 1179 New Star Clusters Found in Gaia DR3
Authors: Huanbin Chi, 焕斌 迟, Feng Wang, 锋 王, Wenting Wang, 雯婷 王, Hui Deng, 辉 邓, Zhongmu Li, 忠木 李
Figure caption: A comparison of different b FoF for five test data sets.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Example X-ray stellar spectra with and without X-ray absorption generated by Lightning. The absorption model used is the tbabs model with Wilms et al. (2000) abundances. The variation in color in the left panel corresponds to a change in the SFH parameters ψ  j  with fixed N H = 1 (× 1020 cm−2). (The age bins for these ψ  j  values are the default set of age bins in Lightning as discussed in Section 2.1.2.) The variation in lines styles in the right panel correspond to changes in N H with fixed ψ  j  = [1, 1, 1, 1, 1] M ⊙ yr−1. The blue line in the left panel shows an example of a spectrum dominated by young stars (i.e., HMXBs), while the red line shows a spectrum dominated by old stars (i.e., LMXBs).
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Examples of the qsosed AGN X-ray emission model connected with the SKIRTOR UV-to-IR model generated by Lightning. The SKIRTOR model shape is fixed using i AGN = 0° and τ 9.7 = 7 with the normalization being set by the qsosed model. The variation in color in the left panel corresponds to a change in ﹩{\mathrm{log}}_{10}\dot{m}﹩ with fixed M SMBH = 108 M ⊙, while different line styles in the right panel correspond to variations in M SMBH with fixed ﹩{\mathrm{log}}_{10}\dot{m}=-1﹩. The light-gray line segments between λ = 2–5 nm (E = 0.24–0.62 keV) show the linear connection of the two models for visualization purposes at the edge of the X-rays. From these examples, it can be seen that ﹩{\mathrm{log}}_{10}\dot{m}﹩ affects the shape of the X-ray emission, while M SMBH mainly affects the normalization.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Examples of the Draine & Li (2007) dust emission model generated by Lightning, normalized by L TIR. The parameters ﹩{U}_{\max }﹩ and α are fixed to 3 × 105 and 2, respectively. The variation in color in the left panel corresponds to a change in ﹩{U}_{\min }﹩ with fixed γ = 0.01 and q PAH = 0.02. The different lines styles in the middle panel correspond to variations in γ with fixed ﹩{U}_{\min }=1﹩ and q PAH = 0.02. As for the right panel, the different symbols on the dotted lines correspond to different values of q PAH with fixed ﹩{U}_{\min }=1﹩ and γ = 0.01. Decreasing the value of ﹩{U}_{\min }﹩ can be seen to shift the peak of the emission to shorter wavelengths, while q PAH independently increases the intensity of the PAH emission features.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Examples of the SKIRTOR AGN emission model generated by Lightning for a range of inclinations with τ 9.7 = 7 normalized by L AGN. The dashed and dashed–dotted lines for the i AGN = 90° example are models where τ 9.7 = 3 and τ 9.7 = 11, respectively. We only show the variation in τ 9.7 for the edge-on example, since τ 9.7 is the edge-on optical depth of the torus. Therefore, changing its value for face-on to moderately inclined viewing angles minimally effects the model.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: The PÉGASE SSP SEDs used in Lightning at various ages after ZAMS for a metallicity of Z = 0.02 and initial mass of 1 M ⊙. For an age of 1 Myr, nebular emission lines can be clearly seen, while the older displayed ages do not have any lines due to our simplifying assumption. Additionally, as the population ages, the overall bolometric luminosity decreases, and the peak wavelength of the emission shifts from the UV into the NIR.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Example modified Calzetti et al. (2000) attenuation curves generated by Lightning, normalized by τ DIFF,V . The black curve gives the base Calzetti et al. (2000) attenuation curve (i.e., δ = 0, τ BC,V  = 0, and no UV bump feature). The variation in color in the left panel corresponds to a change in δ with fixed τ BC,V  = 0, while different line styles in the right panel correspond to variations in τ BC,V  with fixed δ = 0.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Example composite stellar spectrum for a metallicity of Z = 0.02 using the default set of age bins in Lightning. Similarly to the SSPs in Figure 1, the nebular emission lines can be clearly seen in the youngest bin, while the older bins lack any obvious emission features.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: Reconstructed images of GP obtained using scikit-learn. For all three graphs, the different color curves represent the curves of the different kernel reconstructions, the red data points with error bars represent the observed data, and the shaded regions corresponding to the color of the curves indicate the range of 95% confidence intervals of the reconstruction. For each of them, we have the following descriptions: (a) Reconstruction for CC. The horizontal axis z represents the redshift, and the vertical axis H(z) represents the value of the Hubble parameter obtained from the observation. (b) Reconstruction for SNIa (binned). The horizontal axis ﹩\mathrm{ln}(z)﹩ represents the redshift value after logarithmization, and the vertical axis m(z) represents the distance modulus of the supernovae. (c) Plot for reconstruction of GP using the GRB data set. The horizontal axis has the same meaning as in (b). The vertical axis μ(z) represents the distance modulus of the GRB event.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: The Bayes factor between every two kernels is visualized using this heat map to represent the strength of evidence level of the observed data between any two kernels. As an example, the value corresponding to the color block in the second column of the first row on the color bar indicates the Bayes factor of CHY with respect to RBF. That is, P(M CHY∣ y )/P(M RBF∣ y ) (according to Equation (18)). The data set and distance function related to the posterior distribution utilized for the Bayes factor computation for that subplot are indicated in the subplot’s title.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: Bayes factor heat map obtained by direct computation of the evidence. The meaning of each color block is the same as in Figure 3. As an example, for the color block in the second row and first column, the Bayes factor it represents is obtained from ﹩\mathrm{ln}{{ \mathcal Z }}_{\mathrm{RBF}}-﹩                      ﹩\mathrm{ln}{{ \mathcal Z }}_{\mathrm{CHY}}﹩.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: For each subplot, we utilize a bar plot format to display the posterior distribution of the five kernels. The horizontal axis for each subplot denotes the type of kernel, while the vertical axis indicates the likelihood that the observed data are created by them. Normalization is applied to the probability.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: Plots for sampler’s running of three data sets. The horizontal axis of each subplot represents the natural logarithm of the prior volume, ﹩-\mathrm{ln}X﹩. The plot with the vertical axis of ﹩\mathrm{ln}{ \mathcal Z }﹩ is the plot we need for model comparison, and the value that tends to be stable is the model’s corresponding evidence ﹩\mathrm{ln}{ \mathcal Z }﹩.
Paper: Kernel Selection for Gaussian Process in Cosmology: With Approximate Bayesian Computation Rejection and Nested Sampling
Authors: Hao Zhang, Yu-Chen Wang, Tong-Jie Zhang, Tingting Zhang
Figure caption: Visualization plots of evidence in all cases. The solid black line indicates the error bar. The errors are consistent with those given in Table 4. Note that for the CC and GRB data, the log evidence for them is negative.
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 envelope mass within 2500 au (M 2500) with bolometric temperature (T bol) for Aquila (panel (a)) and Orion (panel (b)). Different SED classes are denoted by differently colored open circles as labeled. Filled circles are the PBRSs. The horizontal red bars show T bol bins that are chosen to be equally spaced in log T bol. We use the same T bol bins in both panels: 16, 38, 92, 220, 523, and 1250 K. The vertical red bars denote the interquartile range of M 2500 for the protostars in a particular T bol bin.
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 combined column density–temperature map for the Aquila cloud. The intensity of the map represents the column density of hydrogen, and the color represents the dust temperature. Blue regions are comparatively hotter (>20 K) than red areas (<10 K). The figure shows the structural complexity of the cloud where currently star-forming regions such as Serpens Main and Serpens South are more dense, filamentary, and cold compared to the more evolved regions such as W40. We show the maps for column density and temperature separately in Figure 1 and Appendix B, respectively.
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 total luminosity (L tot) with envelope mass within 2500 au (M 2500) for the eHOPS protostars in Aquila (panel (a)) and HOPS protostars in Orion (panel (b)). Color labels are the same as in Figure 40. M 2500 are chosen to be equally spaced in logarithmic bins. We use the same M 2500 bins in both panels: 0.0002, 0.002, 0.02, 0.2, 2, and 20 M ⊙. The vertical solid bars in each M 2500 bin denote the interquartile range of L tot with the median denoted by open diamonds.
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 L bol for Class 0 protostars (inclusive of PBRSs) and a combined Class I and flat-spectrum sources for Aquila (panel (a)) and Orion (panel (b)). The median L bol for Class 0 protostars in Orion is higher than for the combined Class I and flat-spectrum sources with statistically different distributions. In Aquila, the median L bol for Class 0 is similar to the combined Class I and flat-spectrum sources, with statistically similar distributions.
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 T bol for eHOPS-Aquila (panel (a)), HOPS (panel (b)), and HOPS separately for Orion A and Orion B (panel (c)). The median T bol is shown by the vertical dashed lines, and the first and third quartiles are shown by the vertical dotted lines. The A-D test shows significant differences in the distribution of T bol in Aquila and Orion when protostars in whole clouds are considered, but no significant difference in T bol distribution between Aquila and Orion B.
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: Comparisons of the distributions of M 2500 for protostars in eHOPS-Aquila (panel (a)), HOPS (panel (b)), and HOPS separately for Orion A and Orion B (panel (c)). The first and third quartiles are denoted as Q1 and Q3, respectively. The second quartile (median) is noted in all panels. The A-D test shows a significantly different distribution of M 2500 for protostars in Aquila and Orion. However, the protostars in Orion B have an M 2500 distribution similar to that in 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: The variation of the mid-IR α 4.5,24 with log T bol for Aquila (panel (a)) and Orion (panel (b)). The orange line represents the linear best-fit line with the best-fit relation shown in the legend. We obtain a similar relation in both clouds.
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: The bolometric luminosity vs. temperature (BLT) diagram showing the variation of the bolometric luminosity with the bolometric temperature for the protostars in Aquila (panel (a)) and Orion (panel (b)). Colored open circles denote different SED classes as labeled. Filled circles denote the PBRSs.
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: Positional offset in arcseconds (R.A. in the left panel, and decl. in the right panel) in the sources between Spitzer and Herschel/PACS wavelengths.