adsabs/AstroCLIMB huggingface dataset:
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Left: the satellite stellar-to-halo mass relations obtained in this work: the red curve shows the median relation for our fiducial model described by two parameters and a constant scatter shown in the shaded region (Section 5.1). The blue curve shows the median relation for the growing scatter model described by three parameters (Section 5.2). Right: the same relations compared to recent predictions from previous studies. Garrison-Kimmel et al. (2017) and Nadler et al. (2020) present models obtained using MW satellites, and the Munshi et al. (2021) galaxies are the result of high-resolution hydrodynamical simulations.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Results for the growing scatter satellite–subhalo connection model. Left panel: posterior distribution of the parameters in the growing scatter model for the satellite SHMR. Solid blue lines show the median (50%) and dashed light blue lines show the 68% confidence interval. Right panel: the 68% (blue) and 95% (light blue) confidence intervals for the SSMF predicted by the growing scatter model, compared to the SSMF observed with ELVES (black). The predictions are consistent with the observed SMF and compared to our fiducial model with a constant scatter.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Results for the fiducial satellite–subhalo connection model, assuming a constant scatter. Left panel: posterior distribution of the parameters in the constant scatter SHMR model, derived using 321 satellites and satellite candidates around 27 host galaxies in the Local Volume. Solid red lines indicate the median (50%) and dashed red lines mark the 68% credible interval. See Table 1 for the parameter values. Right panel: the 68% (red) and 95% (light red) credible intervals for the SSMF predicted by the constant scatter model, compared to the SSMF observed with ELVES (black).
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: The methodology used in this work to constrain the satellite SHMR (Section 4.1). We utilized the SatGen model to simulate 50 realizations of the “Local Volume” subhalos around 27 host galaxies (Step 1, Section 3.1). Stellar masses are assigned to dark matter subhalos using a four-parameter SHMR relation (Step 2, Section 4.2), and the stellar mass function is forward modeled to incorporate the observational selection functions and observational incompleteness and uncertainties (Step 3, Section 4.3). In step 4 (Section 4.4), the modeled SSMF is compared to the observed “Local Volume” satellite mass function, and the likelihood for the chosen model parameters is calculated. Steps 2–4 are repeated until the posterior distribution is computed, spanning the predetermined priors.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: The completeness, bias, and scatter as a function of stellar mass, of the ELVES satellite galaxies. The left panel shows the completeness quantified by injecting artificial galaxies into the real survey images. The two rightmost panels show the systematic offset (bias; shown in purple) and the scatter (orange) between the intrinsic (true) and recovered stellar masses. The relations are fitted with a third-order polynomial and used to forward model the SSMF in Section 4.3.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Posterior predictive plots for all 27 ELVES hosts from the stacked Local Volume satellite inference, ranked order by their group K-band magnitude from top left to bottom right. Similarly to Figure 6, the black curves show the SSMF observed with ELVES for each one of the hosts and the colored shaded curves show the 68% and 95% credible intervals for the predicted SSMF, using our constrained fiducial model (5.1) and 50 SatGen realizations for each host. The model describes the data well in the vast majority of cases.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Left panel: the halo mass functions for different “Local Volumes,” each with 27 halos. The halo masses are sampled from a normal distribution around the mean SHMR for massive galaxies from Rodríguez-Puebla et al. (2017) with a constant scatter of 0.15 dex. Right panel: the “total” subhalo mass function using SatGen for all 27 hosts together. The black curve is the median and the shaded black is one standard deviation.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: Forward modeling the SSMF used in inferring the SHMR model parameters. The black curve in all panels shows the observed ELVES SSMF, compared to the colored curves showing the modeled stellar mass functions in each one of the steps. The upper row shows only two such modeled stellar mass functions for clarity whereas the lower row shows all 50 simulated “Local Volumes.”
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: The broad set of observations used to probe the supernova engine. To undertake these studies with a full understanding of the uncertainties involved requires a combination of multiple studies using a variety of codes, implementing different physics in different regimes. Gravitational waves and neutrino emission peak near, or shortly after, core bounce (t 0). Shock breakout occurs t 0 + 30–300 s (Type Ib/c supernovae) or t 0 + ∼10,000 s (Type IIP supernovae). Depending on the amount of asymmetry-driven mixing, MeV gamma rays can rise shortly thereafter (peaking anywhere between 5 days and beyond 100 days.) In the ultraviolet-optical-infrared (UVOIR) bands, shock interactions and shock cooling dominates after shock breakout and peaks at roughly 10–20 days.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption:  U-, V-, R-, K-, and Swift W1-band light curves for both weak (left) and strong (right) supernova explosions from our 15 M ⊙ progenitor. The solid line shows the minimal mixing limited to the inner 0.25 M ⊙ (model M15m0.25f1.0). The dashed line shows the partial mixing throughout the extent of the star (M mix ≈ 13, f mix = 0.25), and the dotted–dashed line shows the full mixing out through the helium core (M mix ≈ 4, f mix = 1.0).
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Distribution of select radioactive isotopes in two supernova explosions of a 15 M ⊙ solar-metallicity progenitor with energies of 0.9 × 1051 erg (left) and 2.6 × 1051 erg (right). 44Ti, 48Cr, and 56Ni all probe the supernova engine. 26Al probes the boundary layer between silicon and carbon/oxygen shells, and neutron-rich iron isotopes, e.g., 59,60Fe, are produced in both the carbon/oxygen and helium shells. Although 26Al and 59,60Fe are all produced in the shell burning prior to collapse, the explosion drives further production and destruction.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Distribution of 44Ti (left) and 56Ni (right) in two different three-dimensional explosions each along three different lines of site. Because of the more asymmetric explosion velocities, there is less of a peak in mass at really low velocities. Clumps of high-velocity ejecta from the supernova engine can escape with higher velocities.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Distribution of select elements in two supernova explosions of a 15 M ⊙ solar-metallicity progenitor with energies of 0.9 × 1051 erg (left) and 2.6 × 1051 erg (right). Although 56Ni probes only the innermost ejecta, a large amount of its ultimate decay product, 56Fe, exists in the solar-metallicity material that forms its stars. Germanium and zinc are also produced in the central engine and are less contaminated by solar abundances.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption:  U-, V-, R-, K-, and Swift W1-band light curves for both weak (left) and strong (right) supernova explosions from our 25 M ⊙ progenitor. The solid line shows the minimal mixing limited to the inner 0.25 M ⊙ (model M25m0.25f1.0). The dashed line shows the partial mixing throughout the extent of the star (M mix ≈ 13, f mix = 0.25). The dotted–dashed line shows this same mixed model but with strong shock heating, where 10% of the kinetic energy is converted to thermal energy.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Mass of 44Ti as a function velocity for a variety of our artificially mixed models. Because of the mass distribution as a function of velocity, even with a fully mixed solution, there is a peak in the mass at low velocities. However, the mass can be spread out to high velocities.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: Moment 0 (integrated intensity) map of the redshifted and blueshifted 13CO (2−1) molecular line emission using the ALMA Band 6 ARI-L data. The redshifted emission (5.99−6.32 km s−1) is shown as red contours. Its contour levels are {−3, 3, 6, 9, ..., 21} × ﹩{\sigma }_{{}^{13}\mathrm{CO}}﹩, where ﹩{\sigma }_{{}^{13}\mathrm{CO}}﹩ is 5.14 mJy beam−1 km s −1. The blueshifted emission (2.67−3.00 km s−1) is shown as blue contours with levels of {−3, 3} × ﹩{\sigma }_{{}^{13}\mathrm{CO}}﹩. The size of the synthesized beam shown in the lower left corner is 1.″255 × 0.″971 (PA = −88°). Gray color scale and black contours denote the 1.3 mm continuum image of the same ARI-L data. Its contour levels are {5, 10, 20, 40, 80, 160} × σ B6, where σ B6 is 223.2 μJy beam−1. The synthesized beam size of the continuum is nearly the same as that of the 13CO (2−1) line emission. Red and blue arrows indicate redshifted and blueshifted outflows, respectively, and the systematic velocity of WL 17 is 4.5 km s−1 (van der Marel et al. 2013). Gray lines indicate the position angles of the disk major and minor axes, 58° and 148°, which are obtained from the ALMA Band 3 continuum image (Figure 1). Note that the redshifted 13CO (2−1) emission is in the southwestern region along the disk major axis, while the blueshifted one is not seen.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: Toomre Q parameter radial profiles of three best-fit models with (a) ﹩{a}_{\max }=1\,\mathrm{cm}﹩ and q = 2.5, (b) ﹩{a}_{\max }=10\,\mathrm{cm}﹩ and q = 3.0, and (c) ﹩{a}_{\max }=10\,\mathrm{cm}﹩ and q = 3.0. To focus on GI in the ring region, these profiles show between 8 and 24 au. In the vertical direction, the black dashed and dotted lines indicate R hole ≃ 16.0 au and σ ring ≃ 3.1 au of the best-fit models, respectively, and the ring region is shown as the shaded region in each panel. In the horizontal direction, the black dashed and dotted lines indicate the critical Toomre Q parameter values of 0.9 (Backus & Quinn 2016) and 1.5 (Boss 2006), respectively, for a protostellar disk around an M-type protostar with 1 M ⊙. The gray shaded regions below these two lines are gravitationally unstable, meaning that Jupiter-mass planet(s) can rapidly form within the ring region.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: Same as Figure 4, but for different models. Contour levels in the Band 7 residual maps are {−39, −24, −12, −6, −3, 3} for model 6, {−24, −12, −6, −3, 3} for model 9, and {−15, −9, −3, 3} for model 12, σ B7 = 0.4 mJy beam−1. Note that these models do not reproduce the Band 7 data well, particularly the central hole.
Paper: 3HWC J0631+107/LHAASO J0631+1040: A TeV Halo Powered by the Pulsar J0631+1036?
Authors: Dong Zheng, Zhongxiang Wang, Yi Xing
Figure caption:  γ-ray spectra of PSR J0631+1036 in its on-pulse data and PS1 in the off-pulse data, with their respective best-fit spectral models also shown. The red long bar indicates the flux upper limit in 0.1–500 GeV at the pulsar’s position derived from the off-pulse data. The HAWC and LHAASO spectral measurements of J0631+107 are shown as the gray and blue shaded regions respectively. Other upper limits shown are on the pulsar (green line) from Archer et al. (2019), on the PWN (two pink lines) from Fernandez-Barral et al. (2017), and in 1–25 TeV on J0631+107 (blue line) from Cao et al. (2023).
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Spectral emission (erg s−1 Å−1) as a function of wavelength (in angstrom) for strong (left) and weak (right) explosions of our 15 M ⊙ progenitor. These models include both a low-mix solution with M mix = 0.25, f mix = 1.0 (solid) and a fully mixed with M mix = 13, f mix = 1.0 solution. The primary feature of the fully mixed solutions is the appearance of heavy metal lines in the early-time UV spectra. At late times, the 56Ni heating in the low-energy explosion alters the spectra dramatically, as it did for the band emission. However, this radioactive heating can be mimicked by shock heating.
Paper: 3HWC J0631+107/LHAASO J0631+1040: A TeV Halo Powered by the Pulsar J0631+1036?
Authors: Dong Zheng, Zhongxiang Wang, Yi Xing
Figure caption: TS maps for the region of PSR J0631+1036 from the whole data (left, in 0.1–500 GeV) and the pulsar’s off-pulse data (middle, in 0.1–500 GeV; right, in 1–500 GeV). The pulsar’s position (pink plus, with the green circle marking its LAT position) is within the 2σ HAWC error circle (the cyan dashed one being 1σ) and the LHAASO 95% error circle (black or white dashed one). Two PSs, PS1 and PS2 (green dashed circles), are marked.
Paper: 3HWC J0631+107/LHAASO J0631+1040: A TeV Halo Powered by the Pulsar J0631+1036?
Authors: Dong Zheng, Zhongxiang Wang, Yi Xing
Figure caption: Comparison of PSR J0631+1036 with Geminga, where the X-ray flux upper limit on the former and measurements of the latter and its PWN, γ-ray pulsar fluxes, and TeV flux measurements of J0631+107 and the TeV halo of Geminga are shown. The fluxes of Geminga are scaled to the distance of PSR J0631+1036.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: X-ray and gamma-ray spectra for five of our mixed explosion models: four models of our strong 15 M ⊙ explosion with different mixing properties and one weak explosion. The shape of the continuum and its evolution allows us to differentiate the different models.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Gamma-ray luminosity (photons above 100 keV) as a function of time for our suite of 15 M ⊙ explosions. The gamma-ray light curve is sensitive to both the extent and amount of mixing. The rise time depends on the extent, and the luminosity depends more sensitively on the amount of mixing. Late-time signals are sensitive to the total 56Ni yield.
Paper: 3HWC J0631+107/LHAASO J0631+1040: A TeV Halo Powered by the Pulsar J0631+1036?
Authors: Dong Zheng, Zhongxiang Wang, Yi Xing
Figure caption: Phase-connected pulse profile (top) and two-dimensional phaseogram (bottom) of J0631+1036 during MJD 54682–57930. Two spin cycles are shown for clarity. The on-pulse and off-pulse phase ranges are marked by dashed lines.
Paper: Multimessenger Diagnostics of the Engine behind Core-collapse Supernovae
Authors: Christopher L. Fryer, Eric Burns, Aimee Hungerford, Samar Safi-Harb, R. T. Wollaeger, Richard S. Miller, Michela Negro, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Bolometric light curves for a sampling of our light-curve models with varying progenitor mass and shock heating (with a few models varying explosion energy and mixing). The breadth of the light curves shows the sensitivity of this emission to shock heating.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: Left: photosphere removal around the [O I] 6300 Å line of the median combined HARPS spectra (black) with a WTTS template (orange). Resultant residual subtraction of the template from the target is shown in blue. Flux values are scaled to the local continuum. Right: corresponding best-fit model to the continuum flux subtracted [O I] line.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: [O I] 6300 Å line luminosity vs. accretion luminosity for PDS 70 and literature values. The accretion luminosity value of PDS 70 is as we measure from the average HARPS spectra emission lines. Markers and colors and the same as Figure 3, as are the sources of literature values.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: [O I] 6300 Å peak velocity vs. FWHM comparing the values we obtain for the fit of PDS 70 to those of other YSOs from the literature values of Manara et al. (2014), Nisini et al. (2018), Fang et al. (2018), and Fang et al. (2023). Points show Class II sources, with TDs indicated by the red circles; blue squares show WTTSs from Upper Sco with detected [O I]. The values we obtained from the best fit of the PDS 70 [O I] is indicated by the green star.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: X-Shooter He I 10830 Å line profiles for each epoch of PDS 70 (black). The best composite-model fit is shown in red, with the maximum blueshifted velocity obtained from the 10% depth of the Gaussian absorption fit shown by the blue circles. The maximum depth of the Gaussian component is shown by the yellow circle. Line profiles are photosphere removed and scaled to the local continuum.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: 47 HARPS epochs of PDS 70 shown in background colors, with median combined spectra shown in thick blue. Flux is scaled to the local continuum and centered around the position of [O I] 6300 Å.
Paper: A Magnetically Driven Disk Wind in the Inner Disk of PDS 70 
Authors: Justyn Campbell-White, Carlo F. Manara, Myriam Benisty, Antonella Natta, Rik A. B. Claes, Antonio Frasca, Jaehan Bae, Stefano Facchini, Andrea Isella, Laura Pérez, Paola Pinilla, Aurora Sicilia-Aguilar, Richard Teague
Figure caption: X-Shooter spectra of PDS70. Epoch 1: 2020-12-24T07:47:32.695. Epoch 2: 2021-02-07T06:37:39.464.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: ALMA Band 3 (3.1 mm; 97.5 GHz) continuum image of the Class I protostellar disk WL 17. Contour levels are {4, 8, 12, 16, 20} × σ B3, where σ B3 corresponds to 33 μJy beam−1. Particularly, the noncircular 8σ B3 contour implies the weak emission in the central hole, which was previously reported in Sheehan & Eisner (2017). The synthesized beam size shown at the lower left is 0.″074 × 0.″060 with PA = 74°. The red plus sign indicates the position of the protostar.
Paper: Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Jaehan Bae, Patrick Sheehan
Figure caption: ALMA images of WL 17. (a) Tapered Band 3 dust continuum image with the synthesized beam of 0.″108 × 0.″103 (PA = 67°) with the sensitivity of 34 μJy beam−1. The red plus sign indicates the position of the protostar. The original Band 3 image is shown in Figure 1. (b) Band 7 dust continuum image with the synthesized beam of 0.″107 × 0.″104 (PA = 67°) with the sensitivity of 0.4 mJy beam−1. Note that substructures are different between Bands 3 and 7. (c) Spectral index (α) map between Bands 3 and 7. The α values are overall small with a mean value of 2.28 ± 0.02, and also they are distributed asymmetrically. (d) Statistical error map of spectral indices. The white contours of panels (c) and (d) mark where the error level is 0.07.