adsabs/AstroCLIMB huggingface dataset:
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Scanning electron microscope (SEM) images of a piece of particle C0002 pressed in indium and location of the SIMS analyses. (A) Backscattered electron (BSE) image of the pressed particle fragment before SIMS analyses. (B) Combined X-ray elemental map of the particle fragment. The particle is dominated by Mg-rich phyllosilicates (purple), sulfides (yellow), and carbonates (light green). Large holes and cracks (black) were avoided for SIMS analyses. (C)–(D) BSE images of areas measured by SIMS. The numbers correspond to the analysis numbers as provided on ORDaR.  Red crosses indicate analyses that were rejected due to small holes or cracks identified by SEM after the SIMS measurements.
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Scanning electron microscope (SEM) images of a piece of particle A0040 pressed in indium and location of the SIMS analyses. (A) Backscattered electron (BSE) image of the pressed particle fragment before SIMS analyses. (B) Combined X-ray elemental map of the particle fragment. The particle is dominated by Mg-rich phyllosilicates (purple), sulfides (yellow), and carbonates (light green). Large holes and cracks (black) were avoided for SIMS analyses. (C)–(D) BSE images of areas measured by SIMS. The numbers correspond to the analysis numbers as provided on ORDaR.                    Red crosses indicate analyses that were rejected due to small holes or cracks identified by SEM after the SIMS measurements.
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Calibration line of the D/H ratios. The calibration includes the different standards analyzed during the session (Table A1) and allows the correction of the instrumental mass fractionation and surface contamination following previous works (Remusat et al. 2016; Piani et al. 2018, 2021).
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Distribution of low-z contaminants that are selected by our photometric dropout and phot-z (p(z > 6.5) > 0.8) selection. Source fluxes are simulated by adding noise to the JAGUAR extragalactic catalogs of three realizations, each of which contains ∼3 × 105 sources over ﹩11^{\prime} \times 11^{\prime} ﹩ area. Noted that scatter points are taken from all simulated fields (﹩\sim 363\,{\mathrm{arcmin}}^{2}﹩ in total; see ﹩4.8\,{\mathrm{arcmin}}^{2}﹩ for each NIRCam module). The estimated number of low-z contaminants per redshift bin per the area of each NIRCam module is shown in the bottom panel. For the cluster field (left), the primary contributors are low-mass (﹩\mathrm{log}{M}_{* }/{M}_{\odot }\sim 7\mbox{--}8﹩) galaxies at z ∼ 2. For the parallel field (right), where only six NIRCam filters are available, the number of contaminants increases. Having more stringent criteria (dashed lines) would help but not completely eliminate such contaminants.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Number density estimates of the F090W-dropout (z ∼ 9, top left panel) and F150W-dropout (z ∼ 12, top right) candidates. Upper limits for the number density of F200W-dropout and F277W-dropout sources, none of which are identified here, are also shown (z ∼ 18, bottom left and z ∼ 24, bottom right). Error bars and upper limits represent 2σ uncertainties. Predicted luminosity functions at the corresponding redshift (Mason et al. 2015, 2023, dashed and dotted lines for the models with and without dust, respectively) shown in each panel.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Star formation rate surface density of our final galaxy candidates plotted as a function of stellar mass (red circles). For comparison, galaxies at 0.2 < z < 4 taken from the 3DHST catalog are shown. Our sample shows a moderate correlation with stellar mass. The measured linear slope (∼0.38; dashed line) is shown.
Paper: Axion-mediated Transport of Fast Radio Bursts Originating in Inner Magnetospheres of Magnetars
Authors: Anirudh Prabhu
Figure caption: Minimum allowed axion–photon coupling consistent with efficiency constraints for a single burst (dashed) and from FRB 121102 (solid) assuming the source is a magnetar with surface field B = 1015 G and rotational period P = 1 s (blue) or P = 1 ms (red). We assume a burst of fluence F = 1 Jy · ms with central frequency ν = GHz and Δν = ν. For the single burst, we have assumed a distance of D = 1 Gpc and conservatively set z = 0. For additional parameter values, see Section 5. We do not consider axion masses less than the plasma frequency of the ISM (see the end of Section 4). We set the fiducial value of the ISM plasma frequency to be that of the Milky Way. Parameter space excluded by other astrophysical probes is shaded (Wouters & Brun 2013; Marsh et al. 2017; Reynolds et al. 2020; Dessert et al. 2020; Sisk-Reynés et al. 2021; Dessert et al. 2022; Noordhuis et al. 2022). QCD axion models are shaded in light purple.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Spectral energy distribution of the final candidates. The best-fit and the 16th–84th percentile range are shown (gray line and hatched region). 2σ error is shown along with the photometric fluxes (red symbols). Blue diamonds represent the model fluxes of the corresponding filter. Photometric-redshift probability distribution (gray for EaZY and red for gsf) is shown in the inset. For those with spectroscopic redshift available (magenta vertical lines in the p(z) panel), redshift is fixed during the SED fitting process. The best-fit model at the secondary peak at low redshift (indicated in the p(z) panel with an arrow) is also shown in the background (orange dashed line). It is noted that fluxes and best-fit parameters are not corrected for lens magnification in the figure.
Paper: Axion-mediated Transport of Fast Radio Bursts Originating in Inner Magnetospheres of Magnetars
Authors: Anirudh Prabhu
Figure caption: Summary of proposed mechanism. Axions (black dashed line) produced at a critical radius in the inner magnetosphere (yellow circle) propagate through the light cylinder (LC) to the dense, preflare wind (purple) and resonantly convert to radio photons (blue wavy line with arrow), which may escape. Relevant length scales are shown at the bottom of the image for a magnetar with rotational period P = 1 s and axion mass m  a  = 10−10 eV. See Section 4 for details of these length scales. The region where an FRB would scatter strongly with the plasma is labeled.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Left: composite RGB image of the Webb’s First Deep Field, in the sightline of SMACS0723 (cluster field). The JWST NIRCam and NIRISS, and HST ACS and WFC3-IR images are combined (blue: F435W+F606W+F814W+F090W+F105W+F115W, green: F125W+F140W+F150W+F160W+F200W, red: F277W+F356W+F444W). The locations of the final high-z galaxy candidates (Section 4.1) are marked. Right: same but for the parallel field (blue: F090W+F150W, green: F200W+F277W, red: F356W+F444W).
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Final color-cut sample (red circles) and phot-z sample (orange circles), shown in two color–color diagrams for F090W-dropout sources (left) and F150W-dropout sources (right). Color tracks of sources at various redshifts are also shown—young galaxy template of different UV β  λ  slopes (blue dashed lines; square symbols mark redshift, starting from z = 7.0 and 11.8 for the left and right panels, respectively, at an increment of Δz = 0.1), low-z early-type galaxy template (red dashed lines), and foreground dwarfs (gray dots).
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Zoom-in image (3.″2 × 3.″2) of the final candidates at z < 12 (in NIRCam F150W) and z > 12 (NIRCam F200W). HST WFC3-IR F160W is shown for those in the cluster field. In the right panel we show the residual image after subtracting a single Sérsic component in the NIRCam image. Surrounding objects are either fitted simultaneously or masked.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Postage stamps of the final color-cut sample (F090W dropouts for the first four and F150W dropouts for the following two). For each object, the top panel shows the image stamps (3.2 × 3.2 arcsec2). “DET” represents the IR-stacked image. The source detection segmentation map and rgb composite (NIRCam F090W/F150W/F200W) image are also shown in the two right panels.
Paper: Physical Characterization of Early Galaxies in the Webb’s First Deep Field SMACS J0723.3-7327
Authors: T. Morishita, M. Stiavelli
Figure caption: Same as Figure 4 but for the phot-z sample. IDs 949 and 963 are analyzed and presented as a single system, ZD6p.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: Bolometric, k-corrected E iso for nearly 150 GRBs compiled from the literature (Abbott et al. 2017; Tsvetkova et al. 2017), with additional bright and faint GRBs compiled following those works and for future analyses. The dashed line is an approximate, empirical detection threshold for GRBs as a function of redshift. Extreme GRBs are highlighted: GRB 130427A, the previous fluence record holder; GRB 090323A, the previous E iso record holder; GRB 111005A, the lowest known E iso for a collapsar; and GRB 170817A, the lowest known E iso overall. GRB 221009A is the record holder.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: Points indicate the annualized logN–logS distributions for GBM, PVO, BATSE, Konus, and Vela. A merged total sample is presented with a fit (from Section 4.1) to the combined logN–logS distribution with index measured as −1.47 ± 0.15 (90% confidence interval). GRB 221009A stands alone, with the Konus and GBM measurements of this burst denoted by stars. A vertical line maps the observed fluence of GRB 221009A to the power-law extrapolation, and the horizontal line marks the inverse recurrence rate of events this bright.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: Bolometric, k-corrected L iso for nearly 100 GRBs compiled from the literature (Abbott et al. 2017; Tsvetkova et al. 2017), with additional bright GRBs compiled following those works. The dashed line is an approximate, empirical detection threshold for GRBs as a function of redshift. Extreme GRBs are highlighted: GRB 110918A and GRB 210619B have higher L iso than GRB 221009A. GRB 160625B is marked, as it is an analog of GRB 221009A, discussed in Section 4.6. We also show GRB 980425, as measured by BATSE, as one of the lowest known L iso values in a GRB. GRB 221009A is not the record holder.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: Points indicate the annualized logN–logP distributions for GBM, PVO, BATSE, and Konus, with peak flux interval indicated in the legend. A power law with fixed index of −3/2 is shown for each separate burst sample. The GBM and BATSE distributions are fit above 1 × 10−5 erg s−1 cm−2; the Konus and PVO distributions are fit above 5 × 10−5 erg s−1 cm−2. GRB 221009A measures are shown with stars, and again it is a significant outlier. The GBM measure of GRB 221009A is faded to indicate that it may be an underestimate.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: The distribution of the ratios of a given GBM peak flux interval against another. Vertical lines denote the median and 1σ bounds for each distribution. The 0.064–0.256 s and 0.256–1.024 s means are nearly identical and overlaid on the figure.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: The probability density funtion of scaling peak flux as measured in a given energy range to the 1 keV−10 MeV bolometric energy range. Note the particularly significant skew in the PVO extrapolation (50–300 keV), which may explain our anomalous PVO peak flux values.
Paper: GRB 221009A: The BOAT
Authors: Eric Burns, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, Stephen Lesage, Yuri Temiraev, Anastasia Tsvetkova, Elisabetta Bissaldi, Michael S. Briggs, Sarah Dalessi, Rachel Dunwoody, Cori Fletcher, Adam Goldstein, C. Michelle Hui, Boyan A. Hristov, Daniel Kocevski, Alexandra L. Lysenko, Bagrat Mailyan, Joseph Mangan, Sheila McBreen, Judith Racusin, Anna Ridnaia, Oliver J. Roberts, Mikhail Ulanov, Peter Veres, Colleen A. Wilson-Hodge, Joshua Wood
Figure caption: The probability density function of scaling fluence as measured in a given energy range to the 1 keV−10 MeV bolometric energy range.
Paper: Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
Authors: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua
Figure caption: 2D distributions of δ∣B∣/δ B against ∣Δv∣/v A in the upstream solar wind, the sheath, and the ICME ejecta, binned across all 74 events. Similar to Figure 3, corresponding 1D distributions are included, the 2D histograms have been normalized to the maximum bin count, and the black lines indicate mean δ∣B∣/δ B with corresponding error estimates. For comparison, the mean ﹩{\sigma }_{{\rm{c}}}^{* }﹩ line from Figure 3 has been superimposed over the distributions in red.
Paper: Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
Authors: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua
Figure caption: 2D distributions of ﹩{r}_{{\rm{E}}}^{* }﹩ against ∣Δv∣/v A, color coded by the mean normalized time from shock (left) and δ∣B∣/δ B (right) of values in each bin. In both histograms, bins containing fewer than five points have been excluded.
Paper: TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars
Authors: Timothy R. Bedding, Simon J. Murphy, Courtney Crawford, Daniel R. Hey, Daniel Huber, Hans Kjeldsen, Yaguang Li, 亚光 李, Andrew W. Mann, Guillermo Torres, Timothy R. White, George Zhou
Figure caption: Pulsation spectra of 35 δ Scuti stars in the Pleiades observed with TESS. Stars are ordered according to the Gaia G BP − G RP color index, whose values are given in parentheses, together with ﹩v\sin i﹩ (if available). Asterisks indicate four stars listed by Heyl et al. (2022) as escaped members. To help guide the eye, the blue dotted lines show approximate frequencies of the first eight radial modes (see Section 6). These are based on the observed frequencies in the star V647 Tau, which has a particularly regular spectrum (Murphy et al. 2022, Table 4).
Paper: TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars
Authors: Timothy R. Bedding, Simon J. Murphy, Courtney Crawford, Daniel R. Hey, Daniel Huber, Hans Kjeldsen, Yaguang Li, 亚光 李, Andrew W. Mann, Guillermo Torres, Timothy R. White, George Zhou
Figure caption: CMD of 89 A and F stars in the Pleiades, based on photometry and parallaxes from Gaia DR3. Photometry has not been corrected for extinction and reddening. (a) Stars are color coded by RUWE (clipped at RUWE = 5 although some stars have greater values), and red circular outlines indicate spectroscopic binaries (Torres et al. 2021); (b) Stars are color coded by ﹩v\sin i﹩ (see Table 1), and red circular outlines indicate five stars listed as escaped members by Heyl et al. (2022). The black line in both panels is a PARSEC isoschrone, corrected for extinction and reddening (see Section 2.).
Paper: TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars
Authors: Timothy R. Bedding, Simon J. Murphy, Courtney Crawford, Daniel R. Hey, Daniel Huber, Hans Kjeldsen, Yaguang Li, 亚光 李, Andrew W. Mann, Guillermo Torres, Timothy R. White, George Zhou
Figure caption: Sample of 89 A and F stars in the Pleiades, of which 36 show δ Scuti pulsations (orange) and 53 do not (blue). (a) CMD, where red circular outlines show the five escaped members (Heyl et al. 2022). For the eclipsing binary V1229 Tau (HD 23642), black circular outlines show (from left to right) the A component (not pulsating), the combined system, and the B component (pulsating; see Section 4.1). The black line is a PARSEC isoschrone (corrected for extinction and reddening; see Section 2). (b) Histogram as a function of Gaia color.