adsabs/AstroCLIMB huggingface dataset:
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: HR diagram, i.e., the luminosity–T eff relation, for the 13 target M dwarfs superimposed on the 5 Gyr theoretical models for [Fe/H] = −0.5, 0.0, +0.5 from the PARSEC library. Models with different ages (0.5 and 10 Gyr) are also plotted in the background for reference, indicating that changes within a reasonable age range do not make a difference in the figure. The black dots and error bars represent the temperature and luminosity recorded in the TIC for the 13 objects. The red arrows on two representative points illustrate the changes that occur when the adopted T eff is adjusted downward by 100 K (see Section 5.2 for a discussion).
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Two examples of atomic lines to show the small difference between the fitting by synthetic spectra and that by Voigt profiles. The data shown by black dots are the observed spectra of ρ Cnc B, the coolest (T eff ∼ 3166 K) target of Ish20. The green solid line and orange dashed line are the best fit by synthetic spectra and Voigt profiles, respectively. Note that the two panels have different scales for both axes.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Sensitivity of EWs of a representative FeH line in model spectra to the adopted T eff. The vertical axis shows the logarithmic EW normalized by the wavelength. Different colors or line styles represent the cases with different metallicities adopted in EW calculation.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: A histogram of the deviation of T eff derived by each FeH line from the mean of T eff derived by all the lines of the corresponding object. The data of all objects are stacked. The red filled histogram is the final case, where we selected 47 FeH lines, and the dashed curve shows a Gaussian fit to it. Also shown as a reference with the histogram outlined in black is the case with 57 FeH lines before the final selection, which deviates from the normal distribution.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Abundance ratios [X/H] of individual elements for each M dwarf as a function of atomic number. The different symbols represent different families of elements: triangles for light odd-Z elements (Na and K), circles for alpha elements, pentagons for iron-peak elements, and diamonds for the neutron-capture element Sr. The error sizes are the σ Total estimated in Section 3. The horizontal dashed line indicates the average of all the elements [Mave/H], weighted by the inverse of the square of the errors.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: The distribution of T eff from TIC of the M dwarfs. The green and red histograms show the samples analyzed in Ish20 and this work, respectively. The sample intentionally contains M dwarfs with T eff > 2800 such that dust formation does not affect the spectra.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Size of errors associated with the resulting [Na/H] caused by individual error sources for each target as a function of [Mave/H] of the objects. The σ SEM is a statistical error. The ﹩{\sigma }_{{T}_{\mathrm{eff}}}﹩, ﹩{\sigma }_{\mathrm{log}g}﹩, and σ  ξ  are errors propagated from the uncertainties of corresponding stellar parameters. The σ OE and σ cont are the errors due to uncertainties of other elements and errors associated with the continuum level uncertainty, respectively. The σ Total is the quadrature sum of all the above errors. The outlier with the smallest error (σ Total ∼ 0.2 dex) is GJ 436, which is due to its higher temperature (T eff ∼ 3456 K) than the other objects.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Iron-normalized abundances of six individual elements in the respective panels as a function of iron abundances. The red stars and green triangles are the M dwarfs analyzed in this work and Ish20, respectively. FGK stars analyzed by Adi12 are displayed as references showing the abundance trends of individual Galactic subpopulations. Among them, the gray dots, pink crosses, and purple circles are the thin disk stars, thick disk stars, and halo stars, respectively.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Iron-normalized abundances of Sr as a function of iron abundances. The red stars are the M dwarfs we analyzed in this work. FGK stars from Mishenina et al. (2019) are displayed as references showing the abundance trends of the thin-disk stars (gray dots) and the thick-disk stars (pink crosses). The cyan open circles represent the nearby early-M dwarfs in Abia et al. (2020).
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Comparison between our resulting [Fe/H] values and the previous estimates of the overall metallicity. The red circles are our results. The purple squares are the estimates by Newton et al. (2014) based on the EW of Na doublet at 2.2 μm. The green triangles and yellow diamonds are the estimates based on the photometric empirical formula of Johnson et al. (2012) and Neves et al. (2012), respectively. The lower six small panels show that the differences between our results and the other estimates as a function of T eff or [Fe/H], where the gray solid lines, gray dashed lines, and orange dashed lines represent the mean, 1σ scatter, and the fitted linear trend, respectively.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Comparison of the [Fe/H] of GJ 699 from our analysis with those from previous studies. The values in the literature are not the iron abundances determined directly only from Fe lines; they refer to overall metallicities, except for that of Maldonado et al. (2020) who empirically determined abundances of iron using principal component analysis and a sparse Bayesian method. The three horizontal dashed lines indicate the result of this study and its 1σ Total range.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Distribution of the 13 M dwarfs in the iron abundance (red histogram in the right panel) and in the error-weighted average of abundances of all the elements (left panel). The black histograms in both panels are the distribution of [Fe/H] values of 1111 FGK dwarfs reported in Adibekyan et al. (2012a), where the [Fe/H] is treated as a proxy for overall metallicity.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: The IRD spectra around a Na I line (1083.78 nm) of M dwarfs at T eff ∼ 3100 K with low metallicity, high metallicity, and metallicity in between.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: The same histograms as in Figure 10 but with 100 K lower T eff adopted.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption: Left: star formation rate and stellar mass distributions of the host galaxies of six repeating and 10 one-off FRBs compared against a population of galaxies at z < 0.6 taken from the PRIMUS survey (Moustakas et al. 2013). Diamond and circle symbols represent the hosts of repeating and nonrepeating FRBs, respectively. The boundary separating the star-forming and quiescent galaxies and its evolution with redshift (Moustakas et al. 2013) is presented by colored dashed lines. Right: rest-frame color–magnitude diagram of the host galaxies of a sample of six repeating and nine one-off FRBs compared to the population of PRIMUS galaxies at z < 0.6. FRB20171020A is not included due to lack of u − r measurement. We also note that the observed magnitudes for FRB20201124A and FRB20200120E are approximated as rest-frame magnitudes because of their low redshifts and, thus, small k-correction. For both plots, the FRB host data is color coded and divided into four redshift bins of <0.0 < z < 0.1 (cyan), <0.1 < z < 0.2 (yellow), <0.2 < z < 0.4 (green), and <0.4 < z < 0.6 (blue).
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption:  REALFAST detection of FRB20180301A. Top and middle panels show the dispersion-corrected frequency-integrated profile and spectrum of FRB20180301A. Bottom panel shows the fast-sampled (10 ms) calibrated radio image of FRB20180301A. The red contour levels are placed at 11.2 mJy beam−1 times factors of [−3, 3, 6, 9, 12, 15, 18]. The synthesized beam in the burst image is 20.″9 × 15.″5 at a position angle of –24.°1.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption:  r-band Gemini image of the host of repeating FRB20180301A and I-band FORS2 images of the hosts of FRB20191228A and FRB20200906A, overplotted with the positions of each FRB. The white solid and dashed circle/ellipse represent the 1σ statistical and systematic uncertainty, respectively, in the FRB position.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption:                         Toomre diagram of our M dwarfs and the FGK stars in Adi12. The types of markers are the same as in Figure 13. The Galactocentric space velocities U, V, and W are with respect to the LSR. Dotted lines represent constant values of the total space velocity ﹩{v}_{\mathrm{tot}}={({U}^{2}+{V}^{2}+{W}^{2})}^{1/2}﹩ in steps of 50 km s−1. The five objects with the lowest [Fe/H] were labeled with names.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption: Redshift distribution of the FRB hosts (red) and PRIMUS sample of field galaxies (dashed black) where the the area under the histogram integrates to 1. The PRIMUS sample lacks good stellar mass and SFR measurements of field galaxies for z < 0.2.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption: Pulse profile and dynamic spectra for FRB20191228A (top) and FRB20200906A (bottom). FRB signals are dedispersed at the S/N maximized DM of 297.5 pc cm−3 and 577.8 pc cm−3 for FRB20191228A and FRB20200906A, respectively.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption: Cumulative distributions of the projected physical offsets, SFRs, stellar masses, metallicities, absolute r-band magnitudes and sSFRs for repeating (blue), nonrepeating (red), and combined (black) FRB host population compared with ultra-luminous X-ray (ULX) sources (cyan), short (light blue), and long (orange) gamma-ray bursts, and core-collapse (CC; green), superluminous (SL; magenta), and Type Ia (brown) supernovae (SNe). The data for these transients are taken from the literature listed in Table 3. The p-value for the KS test between the repeating and nonrepeating population is listed on the right side of each plot. We also summarize the p-values for KS tests between FRB populations and their respective transients in Table 4.
Paper: Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe
Authors: Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, Bing Zhang
Figure caption: Left: cumulative distributions of the host-normalized offsets for FRBs compared with those of Galactic objects in the Milky Way galaxy. The data for various Galactic sources have been taken from Chrimes et al. (2021). The gray-shaded region represents the 1σ uncertainty on the cumulative distribution function, accounting for uncertainties due to individual measurements and sample size. The p-values for KS test between Galactic sources and all FRBs are listed on the right side of the plot. Right: cumulative distributions of the host-normalized offsets for FRBs compared with offset distributions of globular clusters associated with M81, M31 (spiral late-type galaxies), NGC 821 (isolated elliptical galaxy), and NGC 4278 (L* elliptical galaxy). The effective radii used for these galaxies are R eff(M81) = 3.5 kpc (Bhardwaj et al. 2021), R eff(M31) = 7.2 kpc (Savorgnan & Graham 2016), R eff(NGC821) = 5.1 kpc (Pellegrini et al. 2007), and R eff(NGC4278) = 2.4 kpc (Usher et al. 2013). The p-values for KS test between globular clusters and all FRBs are listed on the right side of the plot.