adsabs/AstroCLIMB huggingface dataset:
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: Top panel: best-fit r′- and i′-band light curves in flux space extrapolated from the best-fit bolometric light curve constructed from the A82 model (details in Section 4), assuming the host galaxy extinction is a free parameter between E(B − V)host = 0.3–0.5 mag. The best-fit values are ﹩{M}_{\mathrm{Ni}}={0.18}_{-0.06}^{+0.07}\,{M}_{\odot }﹩, ﹩{\tau }_{{\rm{m}}}={15.98}_{-5.36}^{+2.77}﹩ days, ﹩E{(B-V)}_{\mathrm{MW}}={1.31}_{-0.07}^{+0.06}﹩ mag, ﹩E{(B-V)}_{\mathrm{host}}={0.41}_{-0.07}^{+0.06}﹩ mag, ﹩{m}_{\mathrm{host},\ {\rm{r}}^{\prime} }={24.88}_{-0.07}^{+0.08}﹩ mag, and ﹩{m}_{\mathrm{host},\ i^{\prime} }={23.83}_{-0.12}^{+0.14}﹩ mag. 100 random a posteriori possible models from the MCMC fitting samples are plotted, along with the best fits in bold. Bottom panel: corner plots associated with the MCMC fits of the A82 model, corresponding to the top panel. A total of 33,250 samples were generated in the posteriors.
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: Observed r′- and i′-band photometry of GRB 221009A after T 0 + 1 day, along with the best-fit optical afterglow model corresponding to a power-law decay index of α = 1.434, with the addition of the host galaxy emission. The light curves for a SN 1998bw-like source in the r′ and i′ band, redshifted to z = 0.151 and reddened according to the Galactic and host galaxy extinction of GRB 221009A, are also shown.
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: LDT images of the optical afterglow of GRB 221009A. All of the panels show the position of GRB 221009A circled in pink. The left, large panel shows the wider field of view of GRB 221009A, in r′ band 3.6 days after T 0. The right panels show the evolution over time of the optical afterglow, in both the r′ and i′ bands. The image at 155 days is devoid of afterglow and SN contribution, and the host galaxy is faintly seen in the i′ band. The images have been smoothed for display purposes.
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: the best-fit afterglow+host model, along with its a posteriori possible models and χ values. Right panel: the best-fit SN model, along with its a posteriori models and χ values. The SN model is moderately but not conclusively favored, with a Bayes factor K Bayes = 101.2, and the best-fit parameters for each model are shown in Table 2.
Paper: Magnetar Central Engines in Gamma-Ray Bursts Follow the Universal Relation of Accreting Magnetic Stars
Authors: Simone Dall'Osso, Giulia Stratta, Rosalba Perna, Giovanni De Cesare, Luigi Stella
Figure caption: Left: the universal relation for two different radiative efficiencies, ϵ = 1 (dashed thick line) and ϵ = 0.01 (dashed light-gray line; see Equation (2)). Green dots indicate different classes of accreting compact objects studied by Campana et al. (2018). Colored stars are the GRBs analyzed in this work and for which an isotropically radiating magnetar central engine is assumed. The blue dotted line is the best-fit correlation for the nine GRBs, with a Pearsons correlation coefficient = 0.948 corresponding to a two-tailed p-value for testing a noncorrelation of 9.7 × 10−5. Right: close-up of the left panel, highlighting the GRB population alone. The shaded area around the correlation (blue dotted line) shows the uncertainty in the fit parameters.
Paper: Magnetar Central Engines in Gamma-Ray Bursts Follow the Universal Relation of Accreting Magnetic Stars
Authors: Simone Dall'Osso, Giulia Stratta, Rosalba Perna, Giovanni De Cesare, Luigi Stella
Figure caption: Prompt gamma-ray observed flux light curves from Swift/BAT (15–150 keV) data (with a signal-to-noise ratio of five) for the GRBs in our sample. For each burst, the chosen value of ﹩{F}_{\min }﹩ is indicated by the red, dashed horizontal line while the pink shaded area indicates the uncertainty on ﹩{F}_{\min }﹩, as described in Section 3.1. The gray data points at the end of the two short GRB prompt light curves indicate the flux level obtained from data with a signal-to-noise ratio of four.
Paper: Magnetar Central Engines in Gamma-Ray Bursts Follow the Universal Relation of Accreting Magnetic Stars
Authors: Simone Dall'Osso, Giulia Stratta, Rosalba Perna, Giovanni De Cesare, Luigi Stella
Figure caption: GRB prompt and afterglow luminosity light curves in the (1 keV–10 MeV) and (0.3–30 keV) rest-frame energy range, respectively. The luminosity is corrected for jet beaming. Black vertical dotted lines indicate the temporal window considered for the magnetar model fit. Red dashed–dotted lines indicate, for each GRB, the best-fit magnetar model from which we obtain the magnetic field strength B and spin period P (see Table 2). Horizontal dashed red lines mark the minimum accretion luminosity (﹩{L}_{\min }﹩) before entering the propeller regime, and the pink shading shows the uncertainty on ﹩{L}_{\min }﹩. The latter is wider than the uncertainty on ﹩{F}_{\min }﹩ (Figure 2), due to the added uncertainty on the beaming factor (f  b ).
Paper: Magnetar Central Engines in Gamma-Ray Bursts Follow the Universal Relation of Accreting Magnetic Stars
Authors: Simone Dall'Osso, Giulia Stratta, Rosalba Perna, Giovanni De Cesare, Luigi Stella
Figure caption: Sketch of a GRB light curve in which an accreting magnetic NS switches from accretion to propeller while in the prompt phase, and then to the ejector regime when the afterglow sets in. The vertical span of the shaded band that separates the accretor from the propeller phase corresponds to the gap between the minimum accretion luminosity, ﹩{L}_{\min }﹩, and the maximum propeller luminosity, ﹩{L}_{\mathrm{prop}}^{(\max )}﹩. This gap is expected to be small (∼a few) for millisecond spins. Possible short-term transitions that may take place from the accretion to the propeller regime or vice versa are indicated with a dotted dip or peak in the light curve. The onset of the ejector regime is marked by the early NS spin-down luminosity, L sd. Values on the x- and y-axes are roughly indicative of those of (long) GRBs.
Paper: Magnetar Central Engines in Gamma-Ray Bursts Follow the Universal Relation of Accreting Magnetic Stars
Authors: Simone Dall'Osso, Giulia Stratta, Rosalba Perna, Giovanni De Cesare, Luigi Stella
Figure caption: GRB 091029 light curve from the prompt phase to the end of the plateau. The red dotted–dashed curve shows our model prediction for the minimum accretion luminosity, ﹩{L}_{\min }﹩, the propeller luminosity, the switch on time for the ejector phase (r  m  = r  L ) and the plateau luminosity. Note that this is not a fit, but the curve expected given (﹩{L}_{\min },B,P﹩).
Paper: The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity
Authors: Samuel W. Yee, Joshua N. Winn
Figure caption: Top: Example Monte Carlo sample of planets. The blue histogram is for the disk-driven migration component, obtained by drawing x ≡ a/a R from a shallow power-law distribution (γ 1 = –0.04) truncated at x = 1., blue histogram) The orange histogram is for the high-eccentricity migration component, obtained by drawing x from a steeper power-law distribution (γ 2 = –1.38) truncated at x = 2. Both distributions were further attenuated by the transit probability, R ⋆/a. Bottom: Blue line: the fraction of simulations where the K-S statistic is larger than that for the observed hot Jupiters. Orange line: the fraction of simulations in which the null hypothesis that the period distribution is the same for high- and low-metallicity stars could be ruled out by the K-S test with >95% confidence.
Paper: The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity
Authors: Samuel W. Yee, Joshua N. Winn
Figure caption: Period distributions of hot-Jupiter candidates from the first eight-quarters of the Kepler mission (the same catalog used by Dawson & Murray-Clay 2013). Within the P < 10 day range, the period distribution for planets orbiting metal-rich stars (top) appears distinct from that for metal-poor stars (bottom), but the number of objects is too small to draw any statistical conclusions (K-S test p-value = 0.24). Furthermore, when excluding known false positives (FPs, shaded region), leaving only planet candidates (PCs), the differences between the two distributions are reduced.
Paper: The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity
Authors: Samuel W. Yee, Joshua N. Winn
Figure caption: Left: Period distribution of confirmed hot Jupiters in the NASA Exoplanet Archive orbiting FGK stars brighter than G = 12.0 mag, split by metallicity relative to the median. The metallicities were drawn from the literature (Section 2). Right: Period distribution of an enlarged sample of hot Jupiters with G < 12, split by metallicity relative to the median. In this case, the metallicities are based on calibrated Gaia spectroscopic (GSP-Spec) metallicities (Section 3). In both cases, the observed distribution has a peak at 3–5 days, although we caution that this does not necessarily correspond to a peak in the intrinsic occurrence rate; the distributions were not corrected for detection efficiency. K-S tests do not reject the hypothesis that the period distributions of the metal-poor and metal-rich samples are drawn from the same distribution.
Paper: The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity
Authors: Samuel W. Yee, Joshua N. Winn
Figure caption: The Gaia GSP-Spec metallicities are biased as a function of the inferred metallicity (top left panel). After fitting a linear function to the residuals between the SPOCS and Gaia [M/H] values, the remaining residuals still exhibit a trend as a function of Gaia G BP − G RP color (bottom left panel). We removed this trend by fitting a piecewise linear function with a breakpoint at 0.95. Using the calibration coefficients from a joint fit to these variables, the rms residual between the SPOCS and calibrated Gaia [M/H] values is 0.064 dex (right panels).
Paper: The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity
Authors: Samuel W. Yee, Joshua N. Winn
Figure caption: Estimated 2 hr CDPP values for FGK stars brighter than G = 12 mag observed by TESS in Sector 5 (blue dots), as a function of apparent magnitude. The solid and dashed lines show the 90th and 50th percentiles in magnitude bins of width 0.05. The black and red lines represent high- and low-metallicity subsamples, respectively, divided at the median metallicity of the host sample.
Paper: Wide-binary Stars Formed in the Turbulent Interstellar Medium
Authors: Siyao Xu, Hsiang-Chih Hwang, Chris Hamilton, Dong Lai
Figure caption: Same as Figure 2 but with σ  u  = σ  v /v bon(r) given by σ  v  = 0.7v tur and Equation (1), using M = 2M ⊙, L = 100 pc, V  L  = 10 km s−1, and α = 1/3 as an example. Two different values of r's (as labeled) are considered, with r < r int and r > r int (see Equation (4)), respectively.
Paper: Wide-binary Stars Formed in the Turbulent Interstellar Medium
Authors: Siyao Xu, Hsiang-Chih Hwang, Chris Hamilton, Dong Lai
Figure caption: Initial velocity difference v and separation r between two stars formed in a turbulent environment. As an example, the colored region corresponds to a gravitationally bound system with M = 2M ⊙. The color scale indicates the turbulent speed distribution (Equation (2)). The thick dashed and solid lines correspond to v bon (Equation (3)) and v tur (Equation (1)), respectively. The vertical dashed line corresponds to r int (Equation (4)). The parameters V  L  = 10 km s−1, L = 100 pc, and α = 1/3 are used.
Paper: Wide-binary Stars Formed in the Turbulent Interstellar Medium
Authors: Siyao Xu, Hsiang-Chih Hwang, Chris Hamilton, Dong Lai
Figure caption: Comparison between p(e) derived in this work (solid and dashed–dotted lines, same as in Figure 3) and that taken from Reipurth & Mikkola (2012; RM12). Red dotted line represents the normalized p(e) taken from Reipurth & Mikkola (2012) for the outer binaries in stable bound triples at 1 Myr, with the distribution of semimajor axes of outer binaries peaked around 103 au. Dashed line is the thermal distribution. Blue circles show a power-law fit p(e) ∝ e 1.32 to Gaia wide binaries with separations 103.5–104 au in the Galactic field (Hwang et al. 2022c).
Paper: Wide-binary Stars Formed in the Turbulent Interstellar Medium
Authors: Siyao Xu, Hsiang-Chih Hwang, Chris Hamilton, Dong Lai
Figure caption:  p(e) calculated using Equation (12), where f(u) takes the form in Equation (2) with different values of σ  u  as labeled. The dashed line represents the thermal distribution (p(e) = 2e). The circles correspond to the analytical estimate for σ  u  ≳ 1 given by Equation (13).
Paper: An Independent Determination of the Distance to Supernova SN 1987A by Means of the Light Echo AT 2019xis
Authors: Aleksandar Cikota, Jiachen Ding, Lifan Wang, Dietrich Baade, Stefan Cikota, Peter Höflich, Justyn Maund, Ping Yang
Figure caption: Light echo AT 2019xis observed on 2020 January 3 with FORS2 in the V band (this work), 2020 April 20 with the Multi Unit Spectroscopic Explorer (MUSE; Prog. ID 2104.D-5041(A), PI Kuncarayakti), and 2021 April 12 with the European Southern Observatory (ESO) Faint Object Spectrograph and Camera (EFOSC2) in the V band (as part of PESSTO; Smartt et al. 2015), compared to a Hubble Space Telescope (HST) archival image (Prog. ID. 13401, PI Fransson) observed in the F814W, F606W, and F502N bands with the Wide Field Camera 3 (WFC3). The red lines mark the position of AT 2019xis. The light echo propagated eastward from SN 1987, which is located 4.′05 west from AT 2019xis.
Paper: An Independent Determination of the Distance to Supernova SN 1987A by Means of the Light Echo AT 2019xis
Authors: Aleksandar Cikota, Jiachen Ding, Lifan Wang, Dietrich Baade, Stefan Cikota, Peter Höflich, Justyn Maund, Ping Yang
Figure caption: Distance measurements to SN 1987A determined in this work (cases (i)–(xiii)), compared to the values from the literature. The distances determined by Branch (1987), Hoeflich (1988), Eastman & Kirshner (1989), Hanuschik & Schmidt-Kaler (1991), Schmidt et al. (1992), and Mitchell et al. (2002) are based on the expanding photosphere method, while Panagia et al. (1991), Gould (1994), Gould (1995), and Crotts et al. (1995) derived the distance based on the circumstellar rings. The distance determined by Gould (1995), marked with a triangle, is an upper limit. For the description of cases (i)–(xiii), see Section 3 and Table 2.
Paper: An Independent Determination of the Distance to Supernova SN 1987A by Means of the Light Echo AT 2019xis
Authors: Aleksandar Cikota, Jiachen Ding, Lifan Wang, Dietrich Baade, Stefan Cikota, Peter Höflich, Justyn Maund, Ping Yang
Figure caption: Top left panel: light echo AT 2019xis observed with MUSE on 2020 April 20. The size of the cutout is 4″ × 4″ and is oriented so that north is up and east is left. We measured the image quality FWHM of ∼0.″7 (∼3.6 pixel) using neighboring stars. Top right panel: epoch map of the light echo determined by matching template spectra of SN 1987A to each spaxel. The epochs are given relative to the SN explosion. Bottom panel: an example sequence of the light-echo spectra (red lines) compared to the best-matched SN 1987A templates (black lines). The best-fit epochs are indicated.
Paper: An Independent Determination of the Distance to Supernova SN 1987A by Means of the Light Echo AT 2019xis
Authors: Aleksandar Cikota, Jiachen Ding, Lifan Wang, Dietrich Baade, Stefan Cikota, Peter Höflich, Justyn Maund, Ping Yang
Figure caption: Light curve in the I band (left panel) and polarization measurements (right panel) of the light echo AT 2019xis. Also shown is the simultaneous best fit with the simulated model (blue squares and dashed lines in both panels). The vertical line in the left panel marks the time of the polarization observations, and the triangles are nondetections. The observations shown in this plot were not corrected due to interstellar polarization (ISP) or extinction (see case (i) in Section 3).
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Optical spectrum of the central ∼1 arcsec2 of the host galaxy of FRB 20220912A, PSO J347.2702+48.7066, obtained with Keck I/LRIS. The left panel shows the spectrum in black, the pPXF fit to the stellar continuum in red, and the pPXF fit to the nebular emission lines in cyan. The fit residuals are shown as green points. Selected emission lines are indicated. The middle and right panels show zoomed-in views of certain emission lines (black), with the total pPXF fit in orange.
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Results of a Prospector fit to the optical/IR spectral energy distribution (SED) of the host galaxy of FRB 20220912A, PSO J347.2702+48.7066. The SED measurements from archival PanSTARRS and WISE data are shown in orange, together with representative 10% errors. Filter transmission curves are shown in gray. The maximum a posteriori probability (MAP) model photometry is shown in green, together with the MAP spectrum in red. One hundred spectra generated from draws from the posterior distributions on the model parameters are shown in black.
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Deep optical R-band image obtained with Keck II/ESI (limiting magnitude R ∼ 26) of the localization region of FRB 20220912A. The approximate 90% error ellipse for the DSA-110 localization of FRB 20220912A is shown in white, to the north of the galaxy PSO J347.2702+48.7066.
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Two different verifications of the accuracy with which DSA-110 recovers the positions of known astronomical sources. Both panels show offsets of sources in DSA-110 data from their true positions and the approximate 90% confidence error ellipse quoted for the localization of FRB 20220912A. Top: offsets of sources from cataloged positions in the NRAO VLA Sky Survey (NVSS; Condon et al. 1998) in a 10 min DSA-110 image formed from data taken around Burst 1. Only sources with cataloged flux densities >50 mJy and measured major-axis diameters <30, within 2° of the pointing center, were considered. The symbol size is proportional to flux density. Bottom: offsets of 11 pulses from PSR J1935+1616 localized between 2022 October 22 and 2022 October 25 from the true pulsar position, corrected for proper motion. All pulses were localized using exactly the same pipeline as for the bursts from FRB 20220912A.
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Dedispersed total-intensity dynamic spectra for Bursts 1 (left) and 2 (right) detected with the DSA-110 from FRB 20220912A. Both bursts have been dedispersed to DM = 219.46 pc cm−3. Voltage data in one out of 16 sub-bands for Burst 2 were corrupted, resulting in the blanked data at the top of the band.
Paper: Deep Synoptic Array Science: Discovery of the Host Galaxy of FRB 20220912A
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli, Tomas Ahumada, Dillon Dong, Christoffer Fremling, Yuping Huang, Viraj Karambelkar, Jessie M. Miller
Figure caption: Polarization profiles of bursts 1 (left) and 2 (right) detected by the DSA-110 from FRB 20220912A. Both bursts have been dedispersed to DM = 219.46 pc cm−3. The top panels show the absolute polarization position angle, and Stokes parameters are as labeled in the bottom panels. The polarized dynamic spectra of the bursts were corrected for the small RM reported by CHIME/FRB (0.6 rad m−2).