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Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: NIRSpec image integrated over the wavelength region of [Fe I] 1.443 μm ± 5000 km s−1. This line originates from the ejecta, while the emission from the ER in this wavelength range is due to narrow [Fe I] 1.427 μm and H I 1.460 μm lines, as well as the continuum. The white solid lines show the regions used to extract the spectra of the ejecta (inner ellipse) and ER (elliptical annulus). The white dashed line indicates the approximate area inside which emission from the RS is detected (only a faint continuum component is present at these wavelengths). The dashed black line shows the area affected by light leakage in the long-wavelength ranges of G140M and G235M (see Section 2 and Appendix A). The five point sources seen outside the ER are stars. The ER is inclined by 43°, with the northern part pointing toward the observer.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Images of the [Fe I] 1.443 μm emission from the ejecta as a function of Doppler shift, ranging from V z = –4000 km s−1 (top left) to V z = 5000 km s−1 (bottom right). Each image was integrated over an interval of 500 km s−1. The velocities of freely expanding ejecta in the plane of the sky are shown on the x- and y-axes, where the assumed center of explosion marks 0 velocity (white star symbol). The dashed white line shows the position of the ER.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Spectra of the ejecta (black) and ER (red) extracted from the regions shown in Figure 1. Note that the ejecta region is contaminated by the bright emission from the ER and that some of the ejecta extend into the region of the ER. The strongest lines are identified by the legends, with the color code for different elements and ions given at the top of the figure. All line identifications are also included in Appendix B. Note the broad, boxy line profiles from the RS, best seen in the He I 1.083 μm and Paα 1.875 μm lines. The ejecta spectrum between ∼2.8–3.2 μm in G235M is highly uncertain due to many artifacts in the form of low-valued spaxels.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Volume rendering of the He I 1.083 μm emission from the RS. The two panels show two different viewing angles, as indicated by the arrows in the lower left corners. The emission from the inner ejecta (velocities < 4000 km s−1) has been removed to aid the visualization of the RS. The gray circle shows the position of the ER.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Images of the He I 1.083 μm emission from the RS as a function of Doppler shift. The He I emission from the inner ejecta (velocities < 4000 km s−1) has been removed. The last four panels in the bottom row are contaminated by blended emission from Paγ 1.094 μm and [Si I] 1.099 μm in the ejecta region. The images have been scaled by an asinh function to show the faintest emission more clearly (see color bar). The dashed white line shows the position of the ER and the white star symbol shows the assumed center of the explosion.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Volume rendering of the He I 1.083 μm emission from the RS as in Figure 6, shown together with the ORs (red and blue circles). The left panel has the same viewing angle as the left panel of Figure 6, while the right panel shows the projection on the plane of the sky. The ER is connected to the ORs by dotted lines to aid the visualization.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Median flux of the He I 1.083 μm emission from the RS as a function of the 3D space velocity. The distributions are shown separately for quadrants in the plane of the sky, highlighting the stronger emission in the NE–SW direction and the higher velocities in the SE.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: Left: the locations of KN-associated GRBs on a two-dimensional embedding obtained using PCA-tSNE. The coral-colored labels represent the GRBs with confirmed KN association. The turquoise-colored labels are the GRBs with probable KN candidates. The KN-associated GRBs with long and short duration occupy two locations on the embedding (right and left corners). The filled-grey squares show the location of GRB-SNe on the embedding. Right: same using PCA-UMAP. The embeddings are color coded with respect to the five clusters identified by AutoGMM.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: PCA-tSNE and PCA-UMAP embedding, color coded with T 90 (top) and t mvts (bottom). The encircled regions indicate the locations of KN-associated GRBs in the embeddings.
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: The two FRB sources reported in this work with their respective host galaxies and galaxy clusters. The left column images show filtered ROSAT X-ray intensity (Xu et al. 2022) for galaxy cluster A2310 (top) and A2311 (bottom). The magenta circle in the top left panel has a radius of 1 Mpc and denotes the location of the SZ cluster from the PSZ2 catalog. The bottom panel magenta circle corresponds to our SZ measurement for A2311. The right columns show insets on the position of FRB 20220914A (top) and FRB 20220509G (bottom) plotted over a PanSTARRS1 riz-band image (Chambers et al. 2016, PanSTARRS1).
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Dedispersed total-intensity dynamic spectra for two FRBs detected by DSA-110. Both FRBs reside in galaxies that belong to massive galaxy clusters.
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Slice plots of the smoothed galaxy number density within 5′ of each FRB line of sight. The galaxy data are from the DESI Legacy Imaging Survey DR8 and are mostly photometric redshifts.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: The heatmap illustrates the similarity score between PCA-tSNE and PCA-UMAP embeddings, which is close to 1 for a high value of nearest neighbors. Despite a decrease in score with fewer neighbors, it still stays above 0.5, suggesting that the two embeddings, initialized by PCA, are similar.
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: The polarization properties of FRB 20220509G. The top panel shows a flat PA across the pulse, and the middle panel shows the linearly polarized pulse profile. The bottom panel is the Faraday spectrum with a peak at RM = −111.5 rad m−2.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: The light curves of KN-associated GRBs belonging to various subclusters as identified by AutoGMM.
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Four galaxy clusters from the TNG300-1 simulation whose masses are similar to those of A2310 and A2311. The top row shows gas surface density within 2 Mpc of the cluster center. The green and blue circles represent the impact parameter of FRB 20220509G and FRB 20220914A, respectively. The bottom row shows DMICM as a function of impact parameter, b ⊥, with error bars for the two observed cluster FRBs. The solid purple line is the median DM over fifty azimuthal angles, and the shaded region shows the 90% limits at that b ⊥. The curves assume the FRB is embedded halfway in the ICM, i.e., l LOS = 0.
Paper: Deep Synoptic Array Science: Two Fast Radio Burst Sources in Massive Galaxy Clusters
Authors: Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: The relative probability distributions for each component of the observed FRB DMs. The distributions of DMICM are shown in the purple shaded region under the black curves.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: Top: PCA-tSNE results depicting the two-dimensional embedding (left) and the respective density map (right; bluer regions correspond to a higher density of the bursts clustered at different locations on the map). Bottom: results for PCA-UMAP depicting embedding and density map.
Paper: Evidence for Two Distinct Populations of Kilonova-associated Gamma-Ray Bursts
Authors: Dimple, K. Misra, K. G. Arun
Figure caption: Scree plot presenting the contribution of PCs to explain the variance of the data. The leading four components explain ∼82% of the variance (inset). The first 500 components explain 99% of the variance.
Paper: Origins of the Evil Eye: M64's Stellar Halo Reveals the Recent Accretion of an SMC-mass Satellite
Authors: Adam Smercina, Eric F. Bell, Paul A. Price, Jeremy Bailin, Julianne J. Dalcanton, Roelof S. de Jong, Richard D'Souza, Katya Gozman, In Sung Jang, Antonela Monachesi, David Nidever, Colin T. Slater
Figure caption: Top left: HST photometry from a single ACS field on the outer edge of M64's disk (from PHANGS-HST; Lee et al. 2022). Two distinct populations are visible: the metal-rich disk (red) and a metal-poor accreted component (blue). Best-fit isochrones of [M/H] = −1 and −0.3 are overlaid. Top, second from left: HST photometry converted to g and i filters and degraded to the depth of the Subaru HSC observations. The Subaru RGB selection region and a [M/H] = −1 isochrone model are shown in blue. Sources predicted to be “detected” after applying AST-derived g and i completeness functions are shown as black circles, while sources predicted to be “undetected” are shown in gray. M64's metal-poor halo population is well recovered within our RGB selection region, while the metal-rich disk population is predicted to be largely invisible. Top, third from left: good stellar candidates from Subaru, within the archival ACS field. The RGB is remarkably similar to the predicted CMD of the HST photometry at our Subaru depth, suggesting that our RGB selection criteria are cleanly selecting M64's halo without substantial contamination from the metal-rich disk. Top right: g and i completeness functions for stringently selected RGB candidates in our Subaru HSC observations, derived from ASTs and applied to the HST photometry. Bottom: stellar mass surface density profiles calculated from Subaru RGB counts along the stream (light blue circles), HST metal-poor RGB counts (blue triangles), and HST metal-rich RGB counts (red triangles). A power-law fit to the accreted HST stars is shown. The Subaru minor axis profile and best power-law fit are shown in the inset panel. Corresponding r-band surface brightness, calculated from the same 10 Gyr isochrone used for stellar mass estimation, is shown on the right-hand axis. We also show the integrated light minor axis profile measured by Watkins et al. (2016) for reference (converted using a M/L  V  ratio from Bell & de Jong (2001) and a b/a of 0.57). The profile derived from RGB stars detected with Subaru, in which the shell is clearly visible, matches well the metal-poor halo profile from HST.
Paper: Origins of the Evil Eye: M64's Stellar Halo Reveals the Recent Accretion of an SMC-mass Satellite
Authors: Adam Smercina, Eric F. Bell, Paul A. Price, Jeremy Bailin, Julianne J. Dalcanton, Roelof S. de Jong, Richard D'Souza, Katya Gozman, In Sung Jang, Antonela Monachesi, David Nidever, Colin T. Slater
Figure caption: Top left: Hess CMD in g and r of all sources <1.″5 in size in Fields 1, 2, and 3. The RGB selection region is shown in blue. The considerable contamination from background galaxies and MW foreground stars is clearly visible blueward and above the RGB, respectively. Top center: Color–color diagram of all sources in the southernmost Field 3 (only field with three-filter coverage) <0.″75 in size. The color locus for stars is shown in red. Top right: Hess CMD of the highest-quality stellar candidates in the southern Field 3: sources <0.″75 in size and on the color locus, within photometric uncertainties. Bottom: spatial map of sources <1.″5 in size, within the g − r vs. r RGB selection region. Modest nearest-neighbor filtering has been applied to remove contamination, highlighting the higher-surface brightness structures in M64's halo. The interior of M64 has been filled in with a ground-based image from the Jacobus Kapteyn Telescope (Nik Szymanek, Isaac Newton Group of Telescopes archive).                    A spectacular radial shell feature is visible in the southern halo, with a more diffuse opposing plume extending to the north.
Paper: Origins of the Evil Eye: M64's Stellar Halo Reveals the Recent Accretion of an SMC-mass Satellite
Authors: Adam Smercina, Eric F. Bell, Paul A. Price, Jeremy Bailin, Julianne J. Dalcanton, Roelof S. de Jong, Richard D'Souza, Katya Gozman, In Sung Jang, Antonela Monachesi, David Nidever, Colin T. Slater
Figure caption: Bottom center: gri color mosaic of observations taken with Subaru HSC in the deepest of the three fields, Field 3. M64 is visible at the top of the field, which is ∼115 kpc across at its widest, with much of the diffuse brightness associated with the disk subtracted off as part of the reduction. Obfuscating Galactic cirrus is visible as diffuse filamentary features over much of the field, the color of which complicates inferences of M64's stellar halo from integrated light. The observations are displayed with a logarithmic stretch. Bottom insets: 3′ × 3′ zoomed regions in M64's halo, displayed at the same stretch as the larger image, showing examples of areas dominated by resolved stars at the distance of M64 (left, blue) and background galaxies (right, green). Top right: Color HST image of the inner region of M64 from the Hubble Heritage project.                    M64's dusty inner disk, from which it derives its nickname the “Evil Eye,” is prominent. Top left: H I Moment 1 velocity map, taken from the THINGS survey (Walter et al. 2008). M64's two gas disks are visible, with the larger outer disk rotating counter to the inner disk and the bulk of M64's stars.
Paper: Origins of the Evil Eye: M64's Stellar Halo Reveals the Recent Accretion of an SMC-mass Satellite
Authors: Adam Smercina, Eric F. Bell, Paul A. Price, Jeremy Bailin, Julianne J. Dalcanton, Roelof S. de Jong, Richard D'Souza, Katya Gozman, In Sung Jang, Antonela Monachesi, David Nidever, Colin T. Slater
Figure caption: Left: map of high-quality RGB stars in Field 3, color coded by photometrically inferred metallicity. Nearest-neighbor filtering has been applied to reduce background contamination, as in Figure 2. The chosen shell selection region is shown in red, with the equivalent background region in olive green. The minor axis region is shown in blue and the archival ACS field from PHANGS-HST in magenta. Right: g − i vs. i CMDs of high-quality stellar candidates in the shell (top) and off-shell background (bottom) regions. Stellar isochrones with age 10 Gyr and metallicities from −2 to 0, with 0.25 dex spacing, are overlaid on both. A strong RGB is visible in the shell region, as expected, but is not visible in the background region.
Paper: Origins of the Evil Eye: M64's Stellar Halo Reveals the Recent Accretion of an SMC-mass Satellite
Authors: Adam Smercina, Eric F. Bell, Paul A. Price, Jeremy Bailin, Julianne J. Dalcanton, Roelof S. de Jong, Richard D'Souza, Katya Gozman, In Sung Jang, Antonela Monachesi, David Nidever, Colin T. Slater
Figure caption: Left: map of loosely selected RGB stars in M64's halo (see also Figure 2, bottom), with intensity mapped to stellar density, where each “channel” represents stars in three bins of metallicity: [M/H] ∼ −0.8 (red), [M/H] ∼ −1.2 (green), and [M/H] ∼ −1.7 (blue). Each channel was clipped to two sources per pixel and then smoothed with a Gaussian filter of width ∼1 kpc. The interior of M64 has been filled in with a ground-based image from the Jacobus Kapteyn Telescope. Right: two snapshots from the Aquarius AqF2 simulation presented in Cooper et al. (2011), showing the distribution of accreted stellar material a around a central galaxy of similar mass to M64 during a minor merger with a satellite on a radial orbit. Each snapshot is approximately 80 kpc × 70 kpc. The top panel shows the satellite at first pericenter and the lower panel at a point ∼2 Gyr later. While only qualitative, the lower panel closely resembles the distribution of accreted stars in M64's halo, including its southern shell and northern plume.
Paper: A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A
Authors: Gokul P. Srinivasaragavan, Brendan O'Connor, S. Bradley Cenko, Alexander J. Dittmann, Sheng Yang, Jesper Sollerman, G. C. Anupama, Sudhanshu Barway, Varun Bhalerao, Harsh Kumar, Vishwajeet Swain, Erica Hammerstein, Isiah Holt, Shreya Anand, Igor Andreoni, Michael W. Coughlin, Simone Dichiara, Avishay Gal-Yam, M. Coleman Miller, Jaime Soon, Roberto Soria, Joseph Durbak, James H. Gillanders, Sibasish Laha, Anna M. Moore, Fabio Ragosta, Eleonora Troja
Figure caption: Left panel: modification of Figure 3 from Hjorth (2013), where the flux-stretching factor of the SNe with respect to SN 1998bw (﹩{k}_{\mathrm{SN}\ \,\ 1998\mathrm{bw}}﹩) is plotted against the isotropic-equivalent γ-ray luminosity (L  γ,iso) for their associated GRBs. We distinguish between low-luminosity GRBs, high-energy jet GRBs, and GRBs in the border regime. We indicate the results from this work, GRB 221009A/SN 2022xiw, with a star. We also show the average ﹩{k}_{\mathrm{SN}\ \,\ 1998\mathrm{bw}}﹩ for GRB-SNe in the plot with the exception of GRB 2201009A/SN 2022xiw, along with its dispersion. Right panel: a similar modification of Figure 3 from Hjorth (2013), where the M Ni in M ⊙ of the SNe is plotted against the isotropic-equivalent γ-ray luminosity (L  γ,iso) for their associated GRBs. We make the same distinctions between GRBs as in the above panel, and label the results from GRB 221009A/SN 2022xiw with an upper limit. We also show the average M Ni and dispersion for the GRB-SNe plotted with the exception of GRB 221009A/SN 2022xiw, along with that of the Type Ic-BL sample not associated with GRBs from Taddia et al. (2019).