adsabs/AstroCLIMB huggingface dataset:
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: PPDs of the MCMC analysis for the spectrum from Region A-3 (17:31:23 UT). The red lines represent the fitting results by the nonlinear least chi-square method, while the blue lines are results from the MCMC simulation. The errors are the 1σ confidence intervals of the PPDs. The gray curves in the upper right panels are spectra and residuals associated with results from MCMC samplings shown in the corner plot.
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: PPDs of the MCMC analysis for the spectrum from Region A-2 (17:29:46 UT). The red lines represent the fitting results by the nonlinear least chi-square method, while the blue lines are results from the MCMC simulation. The errors are the 1σ confidence intervals of the PPDs. The gray curves in the upper right panels are spectra and residuals associated with results from MCMC samplings shown in the corner plot.
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: PPDs of the MCMC analysis for the spectrum from Region B-1 (17:26:36 UT). The red lines represent the fitting results by the nonlinear least chi-square method, while the blue lines are results from the MCMC simulation. The errors are the 1σ confidence intervals of the PPDs. The gray curves in the upper right panels are spectra and residuals associated with results from MCMC samplings shown in the corner plot.
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: PPDs of the MCMC analysis for the spectrum from Region A-1 (17:26:36 UT). The red lines represent the fitting results by the nonlinear least chi-square method, while the blue lines are results from the MCMC simulation. The errors are the 1σ confidence intervals of the PPDs. The gray curves in the upper right panels are spectra and residuals associated with results from MCMC samplings shown in the corner plot.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Spectra of SN 2025kg compared to spectra of SN 2006aj (M. Modjaz et al. 2006) and SN 2020bvc (A. Y. Q. Ho et al. 2020) at similar epochs, with times shown in the rest frame. Some host-galaxy lines are clipped for display purposes. The top panel shows the earliest spectrum we have of SN 2025kg along with comparison spectra, and we fit a blackbody to each spectrum to derive temperatures. We find that SN 2025kg has the highest temperature, and a possible broad Fe II feature is beginning to emerge in the spectrum (though we must interpret this with caution, and therefore we do not bold it in the figure; more in Section 3.3), and we also show blueshifted Fe II features in SN 2006aj's and SN 2020bvc’s early-time spectra. The bottom panel shows a spectrum taken at the time of the peak of SN 2025kg in the r band, along with comparison spectra. We see clear blueshifted Fe II and Si II absorption features enabling an SN Ic-BL classification, labeled and shown in bold for SN 2025kg and for SN 2006aj and SN 2020bvc.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: The 10 GHz radio light curve of our VLA nondetections of EP 250108A (green triangles). Also shown are the 8–12 GHz light curves of LLGRB 980425/SN 1998bw (purple; S. R. Kulkarni et al. 1998; E. Waxman et al. 1998), XRF 020903 (pink; A. M. Soderberg et al. 2004), LLGRB 060218/SN 2006aj (orange; A. M. Soderberg et al. 2006), SN 2020bvc (green; A. Y. Q. Ho et al. 2020), and AT 2018cow (yellow; R. Margutti et al. 2019). We additionally plot afterglow models for several pairs of total GRB jet energy (E) and circumburst density (n), generated with the FIREFLY code (R. G. Dastidar & P. C. Duffell 2024) for an on-axis (θobs = 0°; gray) and off-axis (θobs = 30°; black) jet. We cannot rule out radio emission similar to LLGRB 060218/SN 2006aj and SN 2020bvc.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Photospheric velocity evolution for SN 2025kg, compared to other prominent LLGRB SNe (SN 1998bw, K. Iwamoto et al. 1998; SN 2006aj, P. A. Mazzali et al. 2006) and other SNe Ic-BL that likely have different powering mechanisms than just radioactive decay (iPTF 16asu, L. Whitesides et al. 2017; SN 2018gep, A. Y. Q. Ho et al. 2019; SN 2020bvc, A. Y. Q. Ho et al. 2020), with times in the rest frame. SN 2025kg’s vph evolves very similarly to SN 2006aj. The first measurement is shown with an open circle due to the uncertainty in the identification of an Fe II feature (see Section 3.3 for details).
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Comparison of 0.3–10 keV X-ray upper limits of EP250108a/SN 2025kg to the X-ray light curves of GRB 230812B/SN 2023pel (T. Hussenot-Desenonges et al. 2024; G. P. Srinivasaragavan et al. 2024b), LLGRB 060218a/SN 2006aj (S. Campana et al. 2006), LLGRB 980425/SN 1998bw (C. Kouveliotou et al. 2004), double-peaked SN Ic-BL SN 2020bvc (A. Y. Q. Ho et al. 2020), and LFBOT AT 2018cow (L. E. Rivera Sandoval et al. 2018), with times in the rest frame. The WXT detection is also shown, though we show the luminosity in the 0.5–4 keV range. We cannot rule out X-ray emission similar to SN 2006aj or SN 2020bvc.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Fitting of model (b) (collapsar jet-driven shocked cocoon) and the radioactive decay model of W. D. Arnett (1982) in combination with the photometry of SN 2025kg. We show the maximum-likelihood fit and the 90% credible interval.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Fitting of model (c) (collapsar jet-driven shocked cocoon in extended CSM) and the radioactive decay model of W. D. Arnett (1982) in combination with the photometry of SN 2025kg. We show the maximum-likelihood fit and the 90% credible interval.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Fitting of model (a) (SN ejecta–CSM) and the radioactive decay model of W. D. Arnett (1982) in combination with the photometry of SN 2025kg. We show the maximum-likelihood fit and the 90% credible interval.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Corner plots associated with fitting the combined SCE model from A. L. Piro et al. (2021) and the radioactive decay model from W. D. Arnett (1982) to the photometry.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Corner plots associated with fitting the W. D. Arnett (1982) radioactive decay model to the bolometric luminosity LC’s second peak.
Paper: Cosmological Evolution of Fast Radio Bursts and the Star Formation Rate
Authors: Sujay Champati, Vahé Petrosian
Figure caption: (Left) Luminosity–redshift scatter diagram for the mean redshift sample with a linear regression fit (green dashed line) showing a strong luminosity evolution, L ∝ Z7.5, partly due to the truncation shown by the solid black curve based on Equation (5) with ﹩{f}_{{\rm{lim}}}﹩ = 0.5 Jy. (Right) Scatter diagram of the now-independent variables local luminosity, L0, and redshift, Z, with the de-evolved truncation boundary for the mean-Z sample.
Paper: Cosmological Evolution of Fast Radio Bursts and the Star Formation Rate
Authors: Sujay Champati, Vahé Petrosian
Figure caption: (Left) Variation of Kendall’s τ with the index k of the luminosity evolution function (Equation (8)), indicating best (shown by the three solid vertical lines) and 1σ values (shown by the dotted lines only for the mean-Z sample); ﹩k=5.{3}_{-0.2}^{+0.3},6.{1}_{-0.3}^{+0.2},6.{5}_{-0.7}^{+0.2}﹩ for upper- (blue), mean- (black) and lower-Z (red) samples, respectively. (Right) Cumulative local luminosity function for the three samples (upper in blue, mean in black, and lower in red). The lines show the broken power fits based on Equation (13) with parameters given in Table 1.
Paper: Cosmological Evolution of Fast Radio Bursts and the Star Formation Rate
Authors: Sujay Champati, Vahé Petrosian
Figure caption: (Left) Cumulative formation rate numbers for the mean-Z sample. The lower curve (open circles) shows the raw cumulative redshift counts, N(>Z). The middle curve is the correct number counts, including correction for the luminosity evolution. The blue curve is for ignoring luminosity evolution. (Right) Cumulative formation rate numbers for three samples (including luminosity evolution); red for lower, black for mean, and blue for upper, normalized at highest redshift. The curves show the fits obtained using Equation (15).
Paper: Cosmological Evolution of Fast Radio Bursts and the Star Formation Rate
Authors: Sujay Champati, Vahé Petrosian
Figure caption: (Left) Dispersion measure–redshift relation. The points represent the mean values of redshift. The horizontal error bars show the possible lower and upper values, from L. Tang et al. (2023). (Right) Redshift histograms, from L. Tang et al. (2023), for mean-z (top right), upper-z (top left), lower-z (bottom right), and half-lower-z (bottom left) samples. Note that some weaker z < 0.01 are missing from the upper-z sample.
Paper: Cosmological Evolution of Fast Radio Bursts and the Star Formation Rate
Authors: Sujay Champati, Vahé Petrosian
Figure caption: The density rate evolution for three samples (red for lower, black for mean, and blue for upper, with arbitrary normalization) compared to the star formation rate taken from P. Madau & M. Dickinson (2014). The unit on the y-axis applies only to the SFR.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Corner plots associated with fitting the combined shocked cocoon model in an extended CSM from E. Nakar (2015) and the radioactive decay model from W. D. Arnett (1982) to the photometry.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Corner plots associated with fitting the combined shocked cocoon model from E. Nakar & T. Piran (2017) and the radioactive decay model from W. D. Arnett (1982) to the photometry.
Paper: Central Cluster Galaxies: A Hot Spot for Detectable Gravitational Waves from Black Hole Mergers
Authors: Yihao Zhou, Tiziana Di Matteo, Nianyi Chen, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Left: the distribution of the bolometric luminosity of the primary MBH (Lbol,1) and the secondary MBH (Lbol,2) for the foreground event population. The dots are color coded by the observed frequency. The horizontal and vertical black dashed lines mark the AGN luminosity limit: we define an MBH with Lbol > 1043 erg s−1 as an AGN. The red shaded area in the upper right corner represents the dual AGN regions, where both MBHs in the merging pair are AGNs. Dual AGNs comprise 87.4% of the foreground events. The two black shaded areas represent one-AGN regions, for which only one of the MBHs is an AGN, and contain 12.6% of the foreground events. Right: the distribution of the bolometric luminosity Lbol and the merging MBH mass MBH for the dual AGNs at z = 0.3. The blue dots are the whole dual AGN population in ASTRID at the specific redshift. The crosses are the events among the dual AGNs that evolve to be foreground events within 1 Gyr, which are color coded by the observed GW frequency. The two panels share the color bar on the right. For the dual AGN with a mass over 108 M⊙, about 0.7% of them will evolve to CW sources. For dual AGN with MBH > 109 M⊙, NCW/Ndual increases to 8.3%. We show the evolution of NCW/Ndual in the inserted frames: black (red) curve represents the CW fraction for dual AGN with the mass above MBH > 108 (109) M⊙.
Paper: Central Cluster Galaxies: A Hot Spot for Detectable Gravitational Waves from Black Hole Mergers
Authors: Yihao Zhou, Tiziana Di Matteo, Nianyi Chen, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: The properties of foreground events over 100 realizations. Left column: the top panel shows the DP values for each CW source color coded by hc. We highlight the sources with DP > 0.1 (high-DP events) by diamonds. The diamond markers for system 1 and system 2 overlap. The middle/bottom panels show the occurrence rate/DP of the detected CW sources as a function of frequency. In the bottom panel, the gray shaded areas are the 1σ region over 50,000 settings (100 GW sky realizations × 500 sky-position settings; see the Appendix). Right column: from top to bottom, we show the redshift z, the total mass of the merging BHs (Mtot = MBH,1 + MBH,2), and the mass ratio q = MBH,2/MBH,1 for all the CW sources at each frequency. In each panel, the median (blue curves), 1σ intervals (dark shaded area), and 2σ intervals (light shaded area) are plotted. In the right frame of each panel, we show the unweighted (blue), ﹩{h}_{{\rm{c}}}^{2}﹩-weighted (black), and DP-weighted (red) PDF.
Paper: Central Cluster Galaxies: A Hot Spot for Detectable Gravitational Waves from Black Hole Mergers
Authors: Yihao Zhou, Tiziana Di Matteo, Nianyi Chen, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: A visualization of the spatial region around the high-DP event system 3 and system 5 at z = 0.25. These two systems involve a triple merger in the central galaxy of a massive galaxy cluster, which is highlighted by the blue circles. We zoom into a region around it (the orange rectangle), which includes another foreground event (marked by the green circle), and show the gas density field color coded by temperature (red color represents hotter gas). The two small insets on the right show the grz-band flux of the host galaxies of the two CW sources, which are located at the center of the blue/green halos. The position of the merging remnant MBHs is marked by red crosses. The panels in the bottom row illustrate the orbital evolution of the triple merger in system 3 and 5. In each frame, the blue/red/green crosses mark the position of the primary/secondary/third MBH. Their trajectories are plotted with corresponding colors. The black holes involved in the events that are part of the triple merger (system 3 and then system 5) are indicated in the bottom right two panels. In the frames with z ≤ 1, the trajectories are plotted relative to the primary MBH. The underlying field is the star density color coded by the star age, with blue to yellow representing young to old stars.
Paper: Central Cluster Galaxies: A Hot Spot for Detectable Gravitational Waves from Black Hole Mergers
Authors: Yihao Zhou, Tiziana Di Matteo, Nianyi Chen, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: The host galaxy properties of the foreground events (colored dots) compared to all the galaxies in ASTRID (gray pixels). The underlying darker regions represent a higher number density. The dots in the two panels share the same color bar as Figure 4. Upper panels: the projected figures of the host galaxies of the six high-DP CW sources, with the RGB channels representing the flux in the rest-frame grz color bands. Bottom left panel: the distribution of the stellar mass and the central black hole mass in the galaxies. To guide the eye, we add the scaling relation drawn from the observation population in A. E. Reines & M. Volonteri (2015). Bottom right panel: the distribution of the specific star formation rate (sSFR) vs. the stellar mass in the galaxies. In both panels, the black dashed/blue solid curves show the median values for all galaxies/foreground sources. The M⋆,gal is the stellar mass within twice the stellar half-mass radius. The sSFR is measured within a fixed aperture of 20 kpc and averaged over the past 50 Myr.
Paper: Central Cluster Galaxies: A Hot Spot for Detectable Gravitational Waves from Black Hole Mergers
Authors: Yihao Zhou, Tiziana Di Matteo, Nianyi Chen, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: One hundred independent realizations of the low-frequency GW sky based on the mergers in ASTRID. The blue curve represents the median GWB spectra over all realizations, with the inner/outer shaded regions corresponding to 1σ/2σ intervals. Black dots plot the loudest event in each realization at each frequency bin. The foreground events, which have higher hc than the GWB are marked by orange dots. The gray shaded area is the NANOGrav 15 yr GWB. We highlight the events with high DP (with DP > 0.1) using red diamonds. The inset shows the distribution of the chirp mass ﹩{ \mathcal M }﹩ and the luminosity distance DL for all foreground sources, color coded by the observed frequency. The high-DP events, marked by the same index as the GWB plot, are plotted by diamonds.
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: Temporal evolution of polarization maps at 220 MHz for the eastern source during a type III burst. The first column shows Stokes I (total intensity), followed by Stokes Q, U, and V. All of them are in units of kJy/beam. It is evident that at any given time slice these maps show uncorrelated morphologies across Stokes parameters. Notably, at 04:14:14.2 UTC, Stokes Q reverses sign, while Stokes U elongates—behaviors distinct from Stokes I and V, confirming these features as being intrinsic to the solar emission rather than instrumental leakage.