adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Left panels: CO (2–1) and 2 μm zoom-in images of the Northern Arm, Mid-Southwest, Mid-East, and Southern Arm regions (from top to bottom). Hexagons indicate YMCs identified by Whitmore et al. (2023; with numbers indicating their ID from that Letter), YMC-free CO peaks (labeled “CO.N1–N2” and “CO.S1–S3” in Northern and Southern regions, respectively, visually identified from this work), and the galaxy center. The “M2”–“M6” labels indicate YMCs that have a mid-IR counterpart from Galliano et al. (2005). The “J” label indicates that YMC 3 has a radio counterpart from Sandqvist et al. (1995). All images have the same field of view of 10″ (∼950 pc) and color scaling as in Figure 1. Hexagons have the same diameter of 3.″5 (∼330 pc). The black arrows at left indicate the upstream-to-downstream directions. Right panels: CO and C I SLEDs of the hexagons centered at YMCs or YMC-free CO peaks in the corresponding upper/lower four left image panels. Hexagons and SLEDs are color-coded by their R 42 (see the bottom color bar). Solid and dotted lines represent upstream and downstream regions, respectively. The center’s CO SLED is shown as the dashed line in the lower panel. These CO and C I SLEDs are used for the radiative-transfer modeling fitting in Section 3.2, with gas properties reported in Table 2.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Panels (a)–(f): R 42 in red and R CICO in blue as functions of six variables at 330 pc resolution across the inner part of NGC 1365: (a) CO (1–0) line-integrated intensity, (b) velocity dispersion, (c) R 21 line ratio, (d) 2, (e) 11.3, and (f) 21 μm emission. Dashed lines are the best-fit trends and legends show the Spearman’s rank correlation coefficients, which are also reported in Table 1. Each inset upper panel shows the rms distribution of the data after subtracting the best-fit trend in bins of the horizontal-axis variable.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Non-LTE LVG model fitting results for CO and C I SLEDs in hexagon apertures (see Figure 4) in the Northern Arm to Mid-Southwest regions (upper panels) and Southern Arm to Mid-East regions (lower panels), respectively. The x-axis is the azimuthal angle starting clockwise from the PA = 220° direction, same as in Figure 2. Dark/light green and red shadings indicate the θ range of the corresponding regions. The y-axes show (from left to right) gas volume density (﹩\mathrm{log}\,{n}_{{{\rm{H}}}_{2}}﹩), kinetic temperature (T kin), and the [CI/CO] abundance ratio. Hexagon IDs are indicated at the top of the left panels at their corresponding θ. Error bars are the ±1σ uncertainty from the fitting, based on MICHI2 (Liu et al. 2021; see also the Appendix). We discuss the trends of decreasing ﹩\mathrm{log}\,{n}_{{{\rm{H}}}_{2}}﹩ and increasing T kin and [CI/CO] from the upstream (dark green/red, left part of each panel) to the downstream regions (light green/red, right part of each panel) in Section 3.2.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Panels (a)–(d) are the CO (2–1) line-integrated intensity, 2, 11.3, and 21 μm images, PSF-matched to our 3.″5 resolution. A common annulus is shown in all panels with radius =0.9 ± 0.2 kpc, inclination 40°, and PA 220° (white solid line; Lindblad 1999). Panels (e)–(f) show the normalized azimuthal profiles of the four upper panels and R 42, R CICO, and R 21 line ratios as a function of azimuthal angle θ measured from the PA of the receding side of the kinematic major axis. Dark green, light green, dark red, and light red shading represents the Northern Arm, Mid-Southwest, Southern Arm, and the Mid-East regions, respectively.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: YMCs (Whitmore et al. 2023) overlaid on HST RGB (F814W/F555W/F438W) image (top) and JWST F200W (2 μm) image (bottom). All YMCs are shown as red circles. Symbol sizes, from smallest to largest, indicate masses from ∼106.0 M ⊙ to ∼107.1 M ⊙. Cyan squares are YMCs with an age less than ∼3 Myr, and yellow stars are YMCs with an attenuation A  V  > 8 mag. We show these YMCs for the context of the discussion in Section 3.1 of this work. See Whitmore et al. (2023) for the original and detailed study of these YMCs.
Paper: PHANGS–JWST First Results: Variations in PAH Fraction as a Function of ISM Phase and Metallicity
Authors: Jérémy Chastenet, Jessica Sutter, Karin Sandstrom, Francesco Belfiore, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Erik Rosolowsky, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams, Ashley. T. Barnes, Frank Bigiel, Médéric Boquien, Mélanie Chevance, I-Da Chiang, 宜 達 江, Daniel A. Dale, J. M. Diederik Kruijssen, Eric Emsellem, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Kathryn Kreckel, Sharon E. Meidt, Ryan J. Rickards Vaught, Amy Sardone, Eva Schinnerer
Figure caption:  R PAH maps colored by the environmental masks from Querejeta et al. (2021): center in red, bar in green, interarms in gray, spiral arms in blue, and disk in orange. We use this separation to measure the median R PAH in each phase individually, and collectively, in Figure 2.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Upper row: the CO and C I SLED of YMC 29 (M4, the most-excited YMC aperture in the Northern Arm; left panel) and that of YMC 12 (M3, the least-excited YMC aperture in the Mid-Southwest region; right panel). Observed line fluxes are shown as blue squares with error bars. Black to gray solid circles are fitted points from a series of fitting within 1σ with an increasing χ 2 (and reduced χ 2, ﹩{\chi }_{r}^{2}﹩). Bottom panels: corresponding 1/χ 2 distributions of model fitting parameters T kin, ﹩\mathrm{log}\,{n}_{{{\rm{H}}}_{2}}﹩, ﹩\mathrm{log}{N}_{{{\rm{H}}}_{2}}﹩ (nonindependent) and [CI/CO] from the MICHI2 code. Yellow shading indicates the ±1σ parameter range.
Paper: PHANGS–JWST First Results: Variations in PAH Fraction as a Function of ISM Phase and Metallicity
Authors: Jérémy Chastenet, Jessica Sutter, Karin Sandstrom, Francesco Belfiore, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Erik Rosolowsky, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams, Ashley. T. Barnes, Frank Bigiel, Médéric Boquien, Mélanie Chevance, I-Da Chiang, 宜 達 江, Daniel A. Dale, J. M. Diederik Kruijssen, Eric Emsellem, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Kathryn Kreckel, Sharon E. Meidt, Ryan J. Rickards Vaught, Amy Sardone, Eva Schinnerer
Figure caption: Running medians of R PAH as a function of the following: (top left) r/r25; (top right) ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}}),﹩ using metallicity maps from Williams et al. (2022); (middle left) ﹩{I}_{{\rm{H}}\alpha }/{{\rm{\Sigma }}}_{{\rm{H}}{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ in units of ﹩\ \mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{kpc}}^{-2}\,{({M}_{\odot }\,{\mathrm{pc}}^{-2})}^{-1};﹩ (middle right) the fraction of molecular gas; and (bottom left) the environmental masks from Querejeta et al. (2021), with a filled black star showing the median for all pixels within each category. The error bars show 3× SEM in each bin (except for the bottom left panel; only 1 SEM). Note that the middle panels involve the flat HI distribution assumption in IC 5332 and NGC 1365, which may shift the curves horizontally.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Color-composite images produced by J. Schmidt from MIRI data of NGC 628 (top) and IC 5332 (bottom). Red: MIRI F2100W; orange: MIRI F1130W; cyan: MIRI F770W; extra overall brightness in grayscale: MIRI F1000W. The images were used as the models for the first two ESA/JWST Pictures of the Month from the JWST Cycle 1 General Observers Program as featured at https://esawebb.org/images/potm2208a/ and https://esawebb.org/images/comparisons/potm2209a/.
Paper: PHANGS–JWST First Results: Variations in PAH Fraction as a Function of ISM Phase and Metallicity
Authors: Jérémy Chastenet, Jessica Sutter, Karin Sandstrom, Francesco Belfiore, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Erik Rosolowsky, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams, Ashley. T. Barnes, Frank Bigiel, Médéric Boquien, Mélanie Chevance, I-Da Chiang, 宜 達 江, Daniel A. Dale, J. M. Diederik Kruijssen, Eric Emsellem, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Kathryn Kreckel, Sharon E. Meidt, Ryan J. Rickards Vaught, Amy Sardone, Eva Schinnerer
Figure caption: Maps of R PAH in IC 5332 (top left), NGC 628 (top right), NGC 1365 (bottom left), and NGC 7496 (bottom right). We mask the pixels with an S/N < 3 in all bands (gray uniform background). We also mask the central pixels in NGC 1365 and NGC 7496 that are saturated, using instrument PSFs, and perform a by-hand additional masking to remove conspicuous saturation artifacts (shown in gray scale, not included in the analysis). We plot contours for a few of the brightest H II regions. They are clearly visible as depressions (darker colors) in R PAH, especially in NGC 628 and NGC 7496.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Example of a dust-embedded young star cluster, a compact infrared source with no detection in the optical HST images. Postage stamps from all 13 HST+JWST PHANGS images are shown together with photometry as an illustration of the SED fitting that will be performed in the future to constrain the physical properties of these objects.
Paper: PHANGS–JWST First Results: Variations in PAH Fraction as a Function of ISM Phase and Metallicity
Authors: Jérémy Chastenet, Jessica Sutter, Karin Sandstrom, Francesco Belfiore, Oleg V. Egorov, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Erik Rosolowsky, David A. Thilker, Elizabeth J. Watkins, Thomas G. Williams, Ashley. T. Barnes, Frank Bigiel, Médéric Boquien, Mélanie Chevance, I-Da Chiang, 宜 達 江, Daniel A. Dale, J. M. Diederik Kruijssen, Eric Emsellem, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Kathryn Kreckel, Sharon E. Meidt, Ryan J. Rickards Vaught, Amy Sardone, Eva Schinnerer
Figure caption: 2D histograms of the ﹩{I}_{{\rm{H}}\alpha }/{{\rm{\Sigma }}}_{{\rm{H}}{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ and the R PAH, color coded by metallicity, using the gradient from PHANGS–MUSE. The more transparent colors indicate bins with at least 10 hits, while the solid colors indicate those with at least 100 hits per bin.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Same as Figure 7 but for NGC 1365 (top) and NGC 7496 (bottom).
Paper: Multi-messenger Model for the Prompt Emission from GRB 221009A
Authors: Annika Rudolph, Maria Petropoulou, Walter Winter, Željka Bošnjak
Figure caption: Left: Distribution of Lorentz factors of plasma shells launched by the central engine. Here, R ini is the initial radius of a plasma shell. Two cases are shown, respectively leading to high (left axis) and low (right axis) collision radii. The parameter t eng represents the total activity time of the engine, i.e., t eng = t main + t quiet + t late. Middle and right: Two-dimensional phase space of the collision radius and the total energy carried by nonthermal electrons (middle) or the Lorentz factor of the emitting plasma (right). Results are shown for the case of low dissipation radii and SYN-dominated electron cooling (Table 1). The collisions (each represented by a circle) are distinguished by color according to the time interval during which they will be observed: purple (0–36.5 s), blue (36.5–71.5 s), aquamarine (71.5–129.5 s), and green (from 308.5 s). Grouped collisions correspond to four distinctive pulses of the light curve shown in Figure 2.
Paper: Multi-messenger Model for the Prompt Emission from GRB 221009A
Authors: Annika Rudolph, Maria Petropoulou, Walter Winter, Željka Bošnjak
Figure caption: Synthetic light curves for three energy ranges obtained in the “R 16” scenario for the IC- and SYN-dominated cases (in all panels indicated as red and blue curves, respectively; see legend in right panel). In the left panel, we show only the IC-dominated case, as it resembles the SYN-dominated one. We also add observed light curves of Konus  and INTEGRAL SPI-ACS  that operate in a comparable energy range, renormalized to match the same scale and shifted in time to match the same peak times (−175 s for Konus, and −225 s for INTEGRAL SPI-ACS). We set T obs = 0 for the synthetic light curve as the minimum collision time in the observer’s frame.
Paper: Multi-messenger Model for the Prompt Emission from GRB 221009A
Authors: Annika Rudolph, Maria Petropoulou, Walter Winter, Željka Bošnjak
Figure caption: Modeled spectra ﹩{E}_{\mathrm{obs}}{{ \mathcal F }}_{{{\rm{E}}}_{{obs}}}﹩ for the (left) “R 16” and “R 17” (right) scenarios, in both cases, including a SYN- and an IC-dominated scenario (for parameters, see Table 1). Transparent curves correspond to the fluence without taking EBL attenuation into account, and dashed curves to the per-flavor neutrino fluences. The latter are compared with the IceCube upper limit reported in The IceCube Collaboration (2022). The inset shows a zoom-in to the spectrum around the peak in the Fermi-GBM/LAT range (indicated as a shaded region in all plots), with a dotted vertical line at 1060 keV to indicate the position of the observed peak. In the inset we further indicate the photon indices, that are defined of the slope of dN ph/dE obs.
Paper: NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity
Authors: Robert C. Frazier, Gudmundur Stefánsson, Suvrath Mahadevan, Samuel W. Yee, Caleb I. Cañas, Joshua N. Winn, Jacob Luhn, Fei Dai, Lauren Doyle, Heather Cegla, Shubham Kanodia, Paul Robertson, John Wisniewski, Chad F. Bender, Jiayin Dong, Arvind F. Gupta, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Adam Kowalski, Jessica Libby-Roberts, Andrea S. J. Lin, Michael W. McElwain, Joe P. Ninan, Cristobal Petrovich, Arpita Roy, Christian Schwab, Ryan C. Terrien, Jason T. Wright
Figure caption: (a) Diffuser-assisted photometry from APO with the transit model from the joint APO and TESS fit overlaid in blue. The linear model of the airmass is shown in gray. (b) Diffuser-assisted photometry and the joint transit model detrended from the linear model of the airmass. (c) NEID RV data during the transit of TOI-2076 b revealing a clear detection of the RM effect. We attribute the positive slope to stellar activity. (d) NEID RV data detrended from the overall upward slope and the corresponding residuals. (e) Hα index from NEID RV observations. (f) CRX from the NEID RV observations. The data are available as data-behind the figure.(The data used to create this figure are available.)