adsabs/AstroCLIMB huggingface dataset:
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: An example of standard siren H 0 posterior by combining three simulated 1.4–1.4M ⊙ BNS mergers detected by LIGO-Virgo. The blue curve assumes no extra information about the binary viewing angle. The orange curve assumes the viewing angles are constrained accurately with 1σ uncertainty of 5°, and the gray curve assumes the viewing angles are overestimated by 20° (with 1σ statistical uncertainty of 5°). The vertical dashed line indicates the H 0 value chosen for the simulations.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: Probability density distribution of the bias in viewing angle we study in this Letter. The bias for each simulated BNS event is randomly drawn from these distributions.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: Measurements from 10 simulated BNS detections, averaged over 30 realizations. The horizontal axes label the mean (γ 1) of the viewing angle bias distribution. Here we assume the bias follows a Normal distribution centering at γ 1 with a standard deviation of 5°. Left: the median and symmetric 68% credible interval of the H 0 posteriors with (blue) and without (green) applying our mitigation formalism. The red dashed line marks the simulated value of H 0. Right: the median and symmetric 68% credible interval of the inferred bias (β 1) posteriors. The red dashed line represents the line of accurate measurement.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: The median and symmetric 68% credible interval of the H 0 posteriors with (blue) and without (green) applying our mitigation formalism. We assume the viewing angle bias follows a Uniform (top), Poisson (middle), and Exponential (bottom) distribution (see texts for the choices of distribution parameters). These distributions are different from the parameterized model we pick for the bias. The results are measurements from 10 simulated BNS detections, averaged over 30 realizations.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: The difference between the median of the inferred standard deviation (i.e., median of the β 2 posterior) and the standard deviation of the simulated bias when combining 10 simulated BNS events. The data point and error bar show the median and symmetric 68% credible interval of the difference for 30 realizations. The results are for the viewing angle bias following a Uniform (top), Poisson (middle), and Exponential (bottom) distribution.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: The difference between the median of the inferred mean (i.e., median of the β 1 posterior) and the mean of the simulated bias when combining 10 simulated BNS events. The data point and error bar show the median and symmetric 68% credible interval of the difference for 30 realizations. The results are for the viewing angle bias following a Uniform (top), Poisson (middle), and Exponential (bottom) distribution.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: Same as Figure 5 but combining 20 simulated BNS events.
Paper: Mitigating the Binary Viewing Angle Bias for Standard Sirens
Authors: Alberto Salvarese, Hsin-Yu Chen
Figure caption: Same as Figure 7 but combining 20 simulated BNS events.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Effect of potential background secondaries and personal biases of crater statistics on the extraction of production populations. The first column shows the relative SFD, and the second column shows the cumulative SFD constructed using the method introduced in Section 2. (a) and (b) are for crater populations in the northwestern sector (i.e., significantly clustered distribution; black polygon in Figure 1(b)) and eastern sector (i.e., nearly random distribution; blue polygon in Figure 1(b)) of the western mare. (c) and (d) are for crater populations with D ≥ 1 km in the western mare. One population is collected from the large counting area outlined by the blue polygon in Figure 1(b), while the other comes from a more refined, smaller counting area shown in Figure A7.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Independent sketching of counting areas and crater statistics for the western mare at the Chang’E-6 landing region. Red stars are the Chang’E-6 landing site. Counting areas are denoted as the blue polygons. (a) Kaguya TC morning monochrome mosaic. (b) Chang’E-2 orthophoto mosaic. (c) Kaguya MI TiO2 abundance map, stretched in the range of 0 –10 wt%. (d) Clementine color-ratio images. The red, green, and blue channels are the reflectance ratios of 750 nm/415 nm, 750 nm/950 nm, and 414 nm/750 nm, respectively. (e) Locations of impact craters in the seven subareas. Craters with D ≥ 1 km are marked in yellow circles, and others are in red. The base map is the Chang’E-2 orthophoto mosaic. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Incomplete recognition of crater statistics and large uncertainties of diameter measurements using orthophoto maps that were constructed using images with incidence angles of less than 60°. (a) Comparison of number of craters with D ≥ 400 m (n) in a small test area with a size of 967.4 km2. Red circles are craters larger than 600 m in diameter cataloged in this work, and yellow and cyan circles are for the same craters cataloged by X. Zeng et al. (2023) and Z. Yue et al. (2024). The base map is the Kaguya TC morning map. (b) and (c) For the same craters shown in panel (a), diameters measured using the Chang’E-2 orthophoto map are systematically smaller than those measured using the Kaguya TC morning images. The black solid line represents a slope of 1, while the black dashed lines indicate 10% differences in crater diameter measurements between individuals (S. J. Robbins et al. 2014).
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Random distribution of craters with D ≥ 200 m in the yellow polygons shown in Figure 1(a). The Chang’E-6 landing site is marked as a red star. Cells are colored based on the confidence level for the significance of spatial clustering. The intensity of the color deepens as the confidence level increases. Those with a positive z-score and confidence levels above 90% are filled with warm colors, representing significant clustering; those with a negative z-score and confidence levels above 90% are filled with cool colors, representing significant sparse distribution; and those with confidence levels below 90% are filled with white, indicating a nearly random distribution. The base map is the Kaguya TC morning map. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Boundaries of earlier counting areas for the western mare at the Chang’E-6 landing site (red star). The base image (including the color shade) is the spatial clustering map of craters with D ≥ 400 m shown in Figure 1(b). The boundaries are referred or extracted from earlier works.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Areas used to derive the onset diameters of equilibrium on the Chang’E-6 landing mare. (a), (c) and (b), (d) are the morphology of the areas used for crater statistics on the western and eastern mare, respectively. The locations are shown in Figure A3(a). Yellow polygons are counting areas, and red circles are the cataloged craters with D ≥ 75 m. The base image is from the Kaguya TC morning map. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: Left: the F336W – F435W vs. F435W – F814W color–color diagram for compact YMC candidates with S/N > 3 in all three HST UV/optical filters. In dark blue, we overlay the yggdrasil SSP model tracks with solar metallicity and a Kroupa IMF. In red, we overlay the equivalent models using the G. Bruzual & S. Charlot (2003) model tracks. Ages are marked along the sequence. Based on the extinction vector shown in the bottom right, sources that are detected across all three HST filters are primarily YMC candidates with A  V  < 2. Right: the F150W – F200W vs. F200W – F335M color–color diagram for all 3061 compact point sources identified in our JWST NIRCam images (gray). Overlaid in dark blue is the yggdrasil SSP model track adopted here with solar metallicity and a Kroupa IMF. Ages are marked along the sequence. The bottom right arrows represent an extinction of A  V  = 5 and the maximum contribution to the F335M flux from 3.3 μm PAH emission determined for star-forming regions within galaxies observed as part of the PHANGS-JWST survey (K. M. Sandstrom et al. 2023). The red box represents the embedded YMC candidate selection presented in S. T. Linden et al. (2023), where nearly all sources are identified in the JWST imaging alone. In NGC 3256, these candidates all appear to be young(t ≤ 5 Myr) and heavily dust-enshrouded (A  V  = 5−15).
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: Left: a spectral window (1.8–1.92 μm) showing the Paα recombination line for all eight YMCs ordered by their F200W – F335M color with the bluest source at the top and the reddest source at the bottom. The bottom three sources are classified as embedded YMCs based on our color criteria. We see that for these embedded YMCs, multiple H2 (1–0) transitions are found at 1.8358 (S(4)) and 1.892 μm (S(5)), as well as He I at 1.869 μm. The dashed lines represent the background spectra used to subtract the contributions of the surrounding ISM from each YMC spectrum. Right: a spectral window (3–3.5 μm) showing the 3.3 μm PAH emission for the same eight YMCs. We again see that for the reddest YMC candidates with the strongest PAH emission, the H2 (1–0) transition at 3.2350 (O(5)) is easily detected along with the Pfδ recombination line at 3.2961 μm. The dashed lines represent the background spectra extracted for each source.
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: The F335M vs. F200W – F335M color–magnitude diagram with all 3061 compact YMCs detected shown in gray. In dark blue, we plot the yggdrasil SSP model adopted in this analysis along with the same age markers as in the right panel of Figure 2. In dark red, we highlight all 116 embedded YMC candidates based on their F150W – F200W and F200W – F335M colors. In turquoise, we overlay the selection used to identify potential candidates within the NIRSpec field of view (3″ × 3″ ∼ 640 × 640 pc), which have sufficient brightness to extract a high-S/N spectrum from 1 to 3 μm. The bottom right arrow represents the maximum contribution from 3.3 μm PAH emission to the F335M flux observed in K. M. Sandstrom et al. (2023).
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: Top: false-color images of the northern and southern regions of NGC 3256 with both HST (F336W/F435W/F814W) and JWST NIRCam (F150W/F200W/F335M). In turquoise, we overlay the NIRSpec field of view (3″ × 3″ ∼ 640 × 640 pc) of the ERS observations used in this analysis. In black and red, we overlay the apertures for the eight YMC candidates within the selection box in Figure 3 that are sufficiently isolated such that an accurate local background can be determined for each cluster and have sufficient S/N to reliably extract both the Paα and 3.3 μm EWs. Bottom: NIRCam false-color zoom-in images of the field of view of the NIRSpec observations. Red circles represent candidates that fall within the embedded selection based on their F150W – F200W and F200W – F335M colors (see Figures 2 and 3).
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: The F150W – F200W vs. F200W – F335M color–color diagram for all 3061 compact point sources identified in our JWST NIRCam images (gray). Overlaid in dark blue to magenta are yggdrasil SSP model tracks with E(B − V) = 0, 2, 4, 6, and 8. The square points correspond to the eight YMCs selected within our NIRSpec field of view color-coded as in Figure 4. The arrow attached to each point represents the adjusted F200W – F335M color taking into account the measured 3.3 μm PAH EW such that only the stellar emission associated with each source remains. The bottom right arrows represent an extinction of A  V  = 5 and the maximum contribution from 3.3 μm PAH emission to the F335M flux determined for star-forming regions within galaxies observed as part of the PHANGS-JWST survey (K. M. Sandstrom et al. 2023). It is clear that our NIRCam and NIRSpec YMC candidates span nearly an order of magnitude in 3.3 μm PAH strength and the full range of observed F200W – F335M colors in NGC 3256.
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: Left: the Paα EW-derived age vs. the measured F200W – F335M color. We see a clear trend where the reddest YMCs in our sample have the youngest ages as determined from their recombination line EWs. Based on the embedded selection presented in Section 3.3, YMCs in NGC 3256 with F200W – F335M > 0 have ages ≤4 Myr. Middle: the Paα EW-derived age vs. the 3.3 μm PAH EW. We see a clear trend where the YMCs with the strongest PAH emission are also the youngest. Right: the Paα EW-derived age vs. the SED-derived color excess E(B − V). Like in the left panel, we see a clear trend where the most heavily extincted sources (E(B − V) > 3) have the youngest ages (<4 Myr).
Paper: GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256
Authors: Sean T. Linden, Thomas Lai, Aaron S. Evans, Lee Armus, Kirsten L. Larson, Jeffrey A. Rich, Vivian U, George C. Privon, Hanae Inami, Yiqing Song, Marina Bianchin, Thomas Bohn, Victorine A. Buiten, Maria Sanchez-García, Justin Kader, Laura Lenkić, Anne M. Medling, Torsten Böker, Tanio Díaz-Santos, Vassilis Charmandaris, Loreto Barcos-Muñoz, Paul van der Werf, Sabrina Stierwalt, Susanne Aalto, Philip Appleton, Christopher C. Hayward, Justin H. Howell, Matthew A. Malkan, Joseph M. Mazzarella, Eric J. Murphy, Jason Surace
Figure caption: Top: false-color HST imaging of NGC 3256 using F336W (λ = 0.336 μm), F435W (λ = 0.435 μm), and F814W (λ = 0.814 μm). The images are oriented north up and east left, and the 4 kpc scale bar is equivalent to 18″. Bright UV-optically visible clusters are seen predominantly in the dust-free regions of the northern galaxy. These clusters were identified and subsequently characterized in S. Linden et al. (2021). Bottom: false-color JWST NIRCam image of NGC 3256 using F150W, F200W, and F335M observations. The JWST data reveal many bright and red sources previously hidden behind the dust lanes obscuring the southern nucleus and parts of the northern galaxy where UV observations are not able to detect these embedded YMCs. The combination of the JWST filters used in this analysis enables us to characterize the properties of these red sources in NGC 3256 for the first time.
Paper: Discovery of the Binarity of Gliese 229B, and Constraints on the System's Properties
Authors: Samuel Whitebook, Timothy D. Brandt, G. Mirek Brandt, Emily C. Martin
Figure caption: Top: the spectrum of Gliese 229B in the J band between orders 58 and 63 taken in 2022 November. The spectrum is flux-calibrated by a sensitivity function derived from Gl 229A and convolved to a resolution of R ∼ 8000. A Sonora model (M. S. Marley et al. 2021) with T = 850 K and ﹩{\mathrm{log}}_{10}(g/\mathrm{cm}\,{{\rm{s}}}^{-2})=5.0﹩ is overlaid. Middle: the highest resolution R ∼ 25,000 spectrum of Gl 229B from order 59 normalized and shifted to the solar system barycenter rest frame vs. the normalized Sonora model. Bottom: the same full-resolution order 59 spectrum as the middle panel, but for the natural seeing data from 2022 March.
Paper: Discovery of the Binarity of Gliese 229B, and Constraints on the System's Properties
Authors: Samuel Whitebook, Timothy D. Brandt, G. Mirek Brandt, Emily C. Martin
Figure caption: Joint likelihood of orbital period and mass of Gl 229 Bb given our two RV measurements, assuming random eccentricities between 0 and 0.8, random orbital phases and orientations, and a minimum period of 1 day (corresponding to a minimum semimajor axis of ≈1.6 R ⊙). Our two RV measurements confirm that at least ≈15 M Jup of the Gl 229 B system reside in Gl 229 Bb.
Paper: Discovery of the Binarity of Gliese 229B, and Constraints on the System's Properties
Authors: Samuel Whitebook, Timothy D. Brandt, G. Mirek Brandt, Emily C. Martin
Figure caption: Distributions of individual component RVs in both observation epochs derived from bootstrap resampled spectra. Diffracted spectra of Gl 229 A in March provide a consistent but less precise RV, so both epochs of Gl 229 B RVs are compared to that of Gl 229 A from November. The RV of the Gl 229 B system varies by more than 11σ between observations, completely ruling out singularity.
Paper: Discovery of the Binarity of Gliese 229B, and Constraints on the System's Properties
Authors: Samuel Whitebook, Timothy D. Brandt, G. Mirek Brandt, Emily C. Martin
Figure caption: The relative radial velocity of Gl 229B (the RV of Gl 229B minus that of Gl 229A) if the BD is singular. The orbits are drawn from the posterior in G. M. Brandt et al. (2021).
Paper: Massive Star Formation Starts in Subvirial Dense Clumps Unless Resisted by Strong Magnetic Fields
Authors: Ke Wang, Yueluo Wang, Fengwei Xu
Figure caption: (a) Pearson correlation coefficient (P) matrix for the HMSCs. P is in range [−1, 1], where ∣P∣ > 0.6 is considered to show a strong correlation. (b) Comparing the estimated B-field strength to observations. The B est–n relation (blue circles and line) for the HMSCs is fitted as ﹩{B}_{\mathrm{mG}}=0.269\,{n}_{4}^{0.61}﹩, where B mG is B in units of mG and n 4 is ﹩{n}_{{{\rm{H}}}_{2}}﹩ in 104 cm−3. The 288 dust-polarization measurements compiled by J. Liu et al. (2022) are shown in crosses with a fitted line in light blue. The orange line is a fit to Zeeman splitting measurements, with a break at ﹩{n}_{{{\rm{H}}}_{2}}=300﹩ cm−3, adopted from R. M. Crutcher et al. (2010). (c) The discrepancy between gas kinetic temperature and dust temperature. T dust is from J. Yuan et al. (2017), which is derived from SED fitting to Herschel/HiGAL 70–500 μm continuum images at a resolution of 36.″4, comparable to the GBT NH3 data.
Paper: Massive Star Formation Starts in Subvirial Dense Clumps Unless Resisted by Strong Magnetic Fields
Authors: Ke Wang, Yueluo Wang, Fengwei Xu
Figure caption: Overview of an example high-mass starless clump (HMSC) G022.5309-0.1927. (a) Three pseudocolor images with Spitzer maps at 8.0, 4.5, and 3.6 μm (R. A. Benjamin et al. 2003) rendered in red, green, and blue, respectively. (b) Spitzer 24 μm emission (S. J. Carey et al. 2009). (c) Herschel 70 μm emission (S. Molinari et al. 2010, 2016). (d) Herschel 250 μm emission. (e) The dust temperature is shown in background, and H2 column density is shown in gray contours of [2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.0] × 1022 cm−2 (K. A. Marsh et al. 2017). (f) Moment 0 map of NH3(1,1) data of RAMPS shows a good spatial correlation with cold dust emission; the GBT beam size is shown at the bottom left corner. In all panels, the white dashed ellipse outlines the source size.