adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H 0 
Authors: Adam G. Riess, Dan Scolnic, Gagandeep S. Anand, Louise Breuval, Stefano Casertano, Lucas M. Macri, Siyang Li, Wenlong Yuan, Caroline D. Huang, Saurabh Jha, Yukei S. Murakami, Rachael Beaton, Dillon Brout, Tianrui Wu, Graeme E. Addison, Charles Bennett, Richard I. Anderson, Alexei V. Filippenko, Anthony Carr
Figure caption: Comparisons of H 0 between HST Cepheids and other measures (JWST Cepheids, JWST JAGB, and JWST NIR-TRGB) for SN Ia host subsamples selected by different teams and for the different methods. The top section shows the values for H 0 using four geometric anchors and also using only NGC 4258. Below, for each selected subsample (by Team or method), we show the value of H 0 based on the HST Cepheid measurements (from R22) and from the JWST distance measurements. The smaller capped error bars indicate the uncertainty from the distance measures between the first-/second-rung distance measure (Cepheids/TRGB/JAGB) alone, and the full error bar includes the SN data. The CCHP and SH0ES subsamples selected for JWST observations produce a large difference of 3–4  km s−1 Mpc−1 in H 0 a priori owing to selection. The HST Cepheid and JWST distance measurements themselves are in good agreement.
Paper: JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H 0 
Authors: Adam G. Riess, Dan Scolnic, Gagandeep S. Anand, Louise Breuval, Stefano Casertano, Lucas M. Macri, Siyang Li, Wenlong Yuan, Caroline D. Huang, Saurabh Jha, Yukei S. Murakami, Rachael Beaton, Dillon Brout, Tianrui Wu, Graeme E. Addison, Charles Bennett, Richard I. Anderson, Alexei V. Filippenko, Anthony Carr
Figure caption: The main panel compares SN Ia host distances calibrated with NGC 4258 for various distance methods, samples, and telescopes (X-axis) and HST Cepheids (Y-axis). The lower panel shows the differences between these on a per-host basis. The inset shows the mean differences for the whole sample. HST Cepheids are all observed by HST and analyzed by R22 and A. G. Riess et al. (2024); see Table A1 with the mean results given in Table 2. JWST (and specific HST) results can be found either in R24 (corresponding to SH0ES-selected) or F24 (corresponding to CCHP-selected) and computed here from the distances table, Table A2. All measures are in good, ∼1σ, agreement. The largest uncertainties in these comparisons arise from the individual measurements in NGC 4258 and the mean measures of the SN Ia hosts as given in Table 1.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: The orbital period and its derivative (﹩\dot{P}﹩) for all ultracompact binaries in which both are measured (Table 3). Our new systems are highlighted in red. Pure gravitational-wave decay, in the absence of mass transfer and tides, corresponds to ﹩\dot{P}\propto {P}^{-5/3}﹩, which we illustrate for two different chirp masses. All detached systems lie nearly on the same curve of constant chirp mass (﹩{{ \mathcal M }}_{c}=0.32\,{M}_{\odot }﹩), while some accreting systems diverge significantly due to the effects of mass transfer.
Paper: JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H 0 
Authors: Adam G. Riess, Dan Scolnic, Gagandeep S. Anand, Louise Breuval, Stefano Casertano, Lucas M. Macri, Siyang Li, Wenlong Yuan, Caroline D. Huang, Saurabh Jha, Yukei S. Murakami, Rachael Beaton, Dillon Brout, Tianrui Wu, Graeme E. Addison, Charles Bennett, Richard I. Anderson, Alexei V. Filippenko, Anthony Carr
Figure caption: Comparisons of H 0 between HST Cepheids and other subsamples of JWST Cepheids and anchors.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: Left: the mass-loss rate of the progenitor of SN 2022ablq, measured from our stacked Swift XRT observations, for several CSM velocities v  w . The data reveal enhanced mass loss, with rates between 0.05 M ⊙ yr−1 and 0.5 M ⊙ yr−1 during the 0.5–2 yr preceding the explosion, consistent with the X-ray light-curve morphology. Right: the parameter space of B. Margalit et al. (2022), which relates the CSM radii (blue lines) and masses (red lines) to the X-ray light-curve duration (t X) and peak luminosity (L X/ν X), scaled by ﹩\tilde{v}﹩ = v sh/v rad. The CSM configuration inferred for SN 2022ablq is marked with a black star and compared with estimate for SN 2006jc (black circle) and several SNe IIn with well-studied X-ray light curves (P. Chandra et al. 2012; E. O. Ofek et al. 2014; P. Chandra et al. 2015, 2022; P. Chandra 2018, black squares). The SNe Ibn show more confined, lower-mass CSM than the SNe IIn, potentially hinting at different mass-loss rates, timescales, and mechanisms between the progenitors of these classes, although X-ray observations of SNe Ibn at later phases are needed to probe their full CSM distributions.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: The photometric and spectroscopic properties of SN 2022ablq support an SN Ibn classification. Left: the r-band absolute magnitude light curves of SN 2022ablq, the template SN Ibn light curves from G. Hosseinzadeh et al. (2017, green) and S. Khakpash et al. (2024, purple), and the TDE AT2019qiz (M. Nicholl et al. 2020, orange). SN 2022ablq’s light-curve shape is consistent with the SN Ibn templates and inconsistent with the longer-duration light curve of TDEs. Right: optical spectra of SN 2022ablq, Type Ibn SN 2000er, and AT2019qiz. The spectrum of SN 2022ablq before subtracting the host galaxy component is shown in light gray, for comparison with the TDE spectrum. The strong He I emission features dominate the spectra of the SNe Ibn but are not seen in the TDE spectrum.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: The 0.2–10 keV light curve of SN 2022ablq (black), measured from the stacked Swift XRT images, compared with the X-ray light curve of the Type Ibn SN 2006jc (green) from S. Immler et al. (2008). Both X-ray light curves have qualitatively similar shapes, but the emission from SN 2022ablq is more luminous and peaks at an earlier phase. Broken power-law fits to both light curves are shown with dashed gray lines. Rising and declining portions of the light curve are fit separately. The power-law indices reveal an inhomogeneous circumstellar environment for both SNe, with remarkably similar evolution during the rising portion of the light curves.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: The host galaxy properties of SN 2022ablq disfavor an AGN origin to the multiband emission. Left: the locus of star-forming galaxies in the parameter space of J. A. Baldwin et al. (1981) and D. E. Osterbrock & M. M. De Robertis (1985). The properties of SN 2022ablq are measured from an archival SDSS spectrum, compared with literature values (K. N. Abazajian et al. 2009) and cutoffs (L. J. Kewley et al. 2001; G. Kauffmann et al. 2003; K. Schawinski et al. 2007). The host of SN 2022ablq falls outside the cluster of AGN and LINER galaxies (yellow points) in this space, and instead is consistent with an H II galaxy (purple points). Right: ALLWISE and NEOWISE W1 – W2 colors of the host of SN 2022ablq. The explosion epoch of SN 2022ablq is marked with a dashed gray line. The colors fall well below the AGN threshold W1 – W2  > 0.8 mag (Vega magnitudes) during the ∼10 yr before explosion.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: Preexplosion forced photometry at the location of SN 2022ablq from ATLAS and ASAS-SN. Individual epochs have been binned in a 3 day rolling window. Nondetections are shown with lighter-shaded downward-facing triangles and 3σ detections with darker-shaded triangles. Postexplosion photometry from Figure 1 is shown for reference. No significant preexplosion emission is detected for SN 2022ablq; the isolated 3σ detections are more likely statistical, rather than physical, in origin. For comparison we plot r-band precursor detections of the Type Ibn SN 2006jc (pentagons), SN 2019uo (hexagons), and SN 2023fyq (stars). Our forced photometry of SN 2022ablq rules out long-lasting precursors with absolute magnitude M < −14, but are not deep enough to rule out outbursts similar to those of the other SNe Ibn.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: The UV and optical light curves of SN 2022ablq from LCO (circles), ATLAS (pentagons), ASAS-SN (diamonds), and UVOT (squares). Phases are given relative to peak g-band brightness. UVOT and LCO UBV-band photometry is calibrated to Vega magnitudes, while all other photometry is calibrated to the AB system. Offsets are added to each light curve for clarity. The approximate phases of the first three coadded Swift XRT observations are shown by a dashed vertical line—two additional XRT epochs were obtained after SN 2022ablq fell below the detection threshold of our UV and optical observations, and are not displayed here.
Paper: The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission
Authors: C. Pellegrino, M. Modjaz, Y. Takei, D. Tsuna, M. Newsome, T. Pritchard, R. Baer-Way, K. A. Bostroem, P. Chandra, P. Charalampopoulos, Y. Dong, J. Farah, D. A. Howell, C. McCully, S. Mohamed, E. Padilla Gonzalez, G. Terreran
Figure caption: The normalized, host-subtracted spectral time series of SN 2022ablq (black) compared with a representative spectrum of SN 2006jc (green; G. C. Anupama et al. 2009). Phases relative to peak optical brightness (g band for SN 2022ablq and B band for SN 2006jc) are given to the right of each spectrum. Notable spectral features are marked with dashed vertical lines.
Paper: Tracking an Eruptive Prominence Using Multiwavelength and Multiview Observations on 2023 March 7
Authors: Qingmin Zhang, Yudi Ou, Zhenghua Huang, Yongliang Song, Suli Ma
Figure caption: (a)–(b) Temporal evolutions of the deflection angle (blue plus symbols), angular width (green diamonds), r (brown triangles), and total length (orange boxes) of the reconstructed cones, respectively. (c) Temporal evolution of the heliocentric distance of the cones (green circles) and height variations of the bright front of the fanlike CME in the FOVs of LASCO (purple circles) and STA/COR2 (maroon circles). Linear speeds (∼788 and ∼598 km s−1) of the CME throughout the propagation and linear speed (∼680 km s−1) of the prominence after 23:00 UT are labeled. A quadratic polynomial is used to perform curve fitting of h(t) during 20:15−22:30 UT.
Paper: Tracking an Eruptive Prominence Using Multiwavelength and Multiview Observations on 2023 March 7
Authors: Qingmin Zhang, Yudi Ou, Zhenghua Huang, Yongliang Song, Suli Ma
Figure caption: Top panels: the prominence observed by SUVI during 20:28−20:43 UT. Bottom panels: the same EUV images superposed by projections of the cones (cyan dots).
Paper: Tracking an Eruptive Prominence Using Multiwavelength and Multiview Observations on 2023 March 7
Authors: Qingmin Zhang, Yudi Ou, Zhenghua Huang, Yongliang Song, Suli Ma
Figure caption: The CME observed by LASCO-C3 coronagraph during 22:18−23:54 UT and the reconstructed cones for the prominence (magenta dots). The orange arrows point to the CME core. In panel (a), the green arrow points to the bright front of CME.
Paper: Tracking an Eruptive Prominence Using Multiwavelength and Multiview Observations on 2023 March 7
Authors: Qingmin Zhang, Yudi Ou, Zhenghua Huang, Yongliang Song, Suli Ma
Figure caption: Top panels: the prominence observed by EUI during 21:00−21:45 UT. Bottom panels: the same EUV images superposed by projections of the cones (cyan dots).
Paper: Tracking an Eruptive Prominence Using Multiwavelength and Multiview Observations on 2023 March 7
Authors: Qingmin Zhang, Yudi Ou, Zhenghua Huang, Yongliang Song, Suli Ma
Figure caption: The Sun (yellow dots) and reconstructed cones for the prominence (magenta, green, and blue dots) as viewed from Earth (left column), side (middle column), and North Pole (right column) at 20:45 UT (top row), 21:45 UT (middle row), and 23:18 UT (bottom row).
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: Left to right: flux, velocity, and dispersion maps of H2 S(7) (top two rows) and S(1) (bottom two rows) emission lines. Both the main and secondary (outflow) components (see Section 3) are plotted separately. The locations of the nuclei are shown as purple (or white) crosses. The r = 0.″8 apertures used to calculate the H2 gas masses are shown as dotted red, orange, and blue circles in the outflow flux panels. ALMA CO flux contours, with velocities set at ±300 km s−1 (K. Sakamoto et al. 2014), are overplotted as blue and red contours in the outflow velocity (central) panels. The outflowing warm molecular gas is collimated, extends out to a projected distance of ∼600 pc from the S nucleus, and is cospatial with the cold molecular outflow.
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: [Fe II] 1.25 μm/Paβ vs. H2 1–0 S(1) 2.12 μm/Brγ diagram (left) and associated excitation map of the S nucleus (right). Each spaxel in the full NIRSpec FOV on the right is color coded based on a linear fit to the line ratios, as shown in the diagram in the left-hand panel. Data points filled with crosses correspond to spaxels found within the outflow regions, where the cross color identifies whether it is the blue- or redshifted outflow. Median ratio values of the regions within the blue outflow, red outflow, and regions exterior to the outflow are shown as blue, red, and gray stars, respectively. Blue and red contours represent the secondary component (outflows) as traced by the H2 S(1) 17.0 μm line (see Figure 4), while the black contour represents the PAH 3.3 μm emission, set at 1.0, 5.0, and 10.0 × 10−19 W m−2. The white cross at the center marks the location of the S nucleus. The regions where we detect the secondary H2 components (outflows) tend to have higher [Fe II]/Paβ and H2/Brγ ratios that are not seen in the regions surrounding the S nucleus.
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: Center: H2 S(1) 17.0 μm velocity maps (in units of km s−1) of the main and secondary (outflow) gas components, where the main component is defined as the emission profile closest to the systemic velocity. Flux contours (1.0, 8.0, and 10.0 × 10−20 W m−2) of the H2 S(1) outflow component are overplotted in red and blue, and the purple crosses are the locations of the nuclei. The full spatial extent of the outflows based on our detection thresholds are plotted in the central-right velocity map (with an adjusted color scale). Upper right: NIRCam F200W image with the spatial coverage of the velocity map (MIRI channel 3 FOV) is overplotted. Left and right: aperture extractions (r = 0.″4) of the normalized S(1) emission at various locations (A–E) are overplotted in the velocity map of the main component and show the diverse emission profiles. The vertical dotted line represents the rest-frame wavelength of S(1). The best-fit model is plotted for each extraction, where the green line represents the main component fit, and the blue and red filled Gaussians represent the blueshifted and redshifted outflow components, respectively. The majority of the outflowing components are spectrally resolved from the main component and show the structure extending to the north and south from the S nucleus.
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: H2 S(7)/S(1) flux ratio map. The purple crosses indicate the locations of the two nuclei, and the apertures used to calculate the masses and power-law indices of the secondary component are shown as dashed circles. We see higher ratios, indicating a larger fraction of warmer gas, closer to the S nucleus, suggesting that the heating of the H2 is caused by it. We also measure slightly higher average ratios in the southwards, blueshifted gas than the northwards, redshifted gas. Lastly, the temperature distribution within the apertures are indicative of a larger warm gas fraction in blueshifted gas.
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: Excitation diagram of the blue and redshifted gas using the r = 0.″8 apertures, as shown in Figure 4. Plotted are the column densities (N) of the H2 S(8)–S(1) transitions, normalized by their statistical weight, g, as a function of their energy level E. The N/g ratios are normalized with respect to the S(1) transition. The best fits to the redshifted (northern and southern regions) and blueshifted gas are denoted by the dashed red, orange, and solid blue lines, respectively. H2 S(3), S(6), and S(8) emission were not included in the southern portion of the redshifted gas due to not passing our S/N > 5 detection threshold. The errors are comparable to the symbol size. The lower power-law index of the blueshifted gas indicates that it has a larger warm gas mass fraction. In addition, the fraction of warm gas seems to be higher closer to the nucleus.
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: Middle left: JWST/NIRCam false-color image of NGC 3256 using the F150W (1.5 μm), F200W (2.0 μm), and F444W (4.4 μm) filters. Top left and bottom left: NIRSpec G235H/F170LP 2 μm continuum images of each nucleus are also shown (field-of-view (FOV) size). These images correspond to the locations indicated by the cyan boxes in the NIRCam image. Right: full NIRSpec spectra (0.97–5.27 μm), which were extracted from the nuclear (black) and off-nuclear (blue) regions using a 0.″2 radius aperture (top for the N nucleus and bottom for the S nucleus). Their extraction locations and sizes are indicated with the same color in the top-left and bottom-left images, and the spectra shown here have been corrected for aperture losses. The S nucleus is heavily obscured, significantly redder in the MIR, and has strong 3.05 μm H2O and 4.27 μm CO2 ice absorption.