adsabs/AstroCLIMB huggingface dataset:
Paper: Rest-frame UV Colors for Faint Galaxies at z ∼ 9–16 with the JWST NGDEEP Survey
Authors: Alexa M. Morales, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Nikko J. Cleri, Romeel Dave, Mark Dickinson, Henry C. Ferguson, Nimish P. Hathi, Ewan Jones, Anton M. Koekemoer, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Britton Smith, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Top: Rest-UV magnitude (M UV) vs. rest-frame UV spectral slope (β) for simulated galaxies at z = 9 and 11. Our results from SED fitting (cyan circles) are compared to simulations and observational works from others. The green line marks the median, and the shaded area marks the 16th and 84th percentiles for galaxies in bins of M UV galaxies predicted by SC-SAM with merger trees from GUREFT (Yung et al. 2024, 2023), FLARES (pink median track with shaded 16th and 84th percentiles; Lovell et al. 2021; Vijayan et al. 2021; Wilkins et al. 2023), SIMBA-EOR (purple median track with shaded 16th and 84th percentiles; Davé et al. 2019; E. Jones et al. 2024, in preparation), Austin et al. (2023; diamond), Tacchella et al. (2022; star), Cullen et al. (2023b; triangle), and Topping et al. (2022; square). Bottom: Stellar mass, log(M */M ⊙), vs. rest-frame UV spectral slope (β) for observed and simulated galaxies at z = 9 and 11. All data points and tracks are denoted in a similar manner to the top panels. The green line marks the median, and the shaded area marks the 16th and 84th percentiles for galaxies in bins of M * from GUREFT, FLARES (pink median track with shaded 16th and 84th percentiles; Lovell et al. 2021; Vijayan et al. 2021; Wilkins et al. 2023), SIMBA-EOR (purple median track with shaded 16th and 84th percentiles; Davé et al. 2019; E. Jones et al. 2024, in preparation), this work (cyan circles), Austin et al. (2023; diamond), Tacchella et al. (2022; star), and Topping et al. (2022; square).
Paper: Rest-frame UV Colors for Faint Galaxies at z ∼ 9–16 with the JWST NGDEEP Survey
Authors: Alexa M. Morales, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Nikko J. Cleri, Romeel Dave, Mark Dickinson, Henry C. Ferguson, Nimish P. Hathi, Ewan Jones, Anton M. Koekemoer, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Britton Smith, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: UV spectral slopes, β, as a function of redshift (color-coded by rest-UV apparent magnitude, mAB, defined at λ rest = 1500 Å) from this work are shown as circles. Squares are from Topping et al. (2022), stars are from Tacchella et al. (2022), triangles are from Cullen et al. (2023b), and diamonds are from Austin et al. (2023). The black line and shaded region at β SED = −2.51 ± 0.07 is the baseline spectral slope for halos enriched by only Population III stars from Jaacks et al. (2018). This work is consistent with the works of others; however, no clear trends are shown with UV spectral slope as a function of redshift when all data are combined. The corresponding Spearman R correlation coefficient is listed for this work only in the lower right corner. Within our sample, we see no evidence for ultrablue UV spectral slopes.
Paper: Rest-frame UV Colors for Faint Galaxies at z ∼ 9–16 with the JWST NGDEEP Survey
Authors: Alexa M. Morales, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Nikko J. Cleri, Romeel Dave, Mark Dickinson, Henry C. Ferguson, Nimish P. Hathi, Ewan Jones, Anton M. Koekemoer, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Britton Smith, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: UV β slope as a function of dust attenuation, SFR, and age (color-coded by redshift). The black line and shaded region at β SED = −2.51 ± 0.07 is the baseline spectral slope for halos enriched by only Population III stars from Jaacks et al. (2018). SFR, dust attenuation, and age show a moderately positive correlation with β. The corresponding Spearman R correlation coefficients are listed for each parameter in the upper left corner of each panel.
Paper: Rest-frame UV Colors for Faint Galaxies at z ∼ 9–16 with the JWST NGDEEP Survey
Authors: Alexa M. Morales, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Nikko J. Cleri, Romeel Dave, Mark Dickinson, Henry C. Ferguson, Nimish P. Hathi, Ewan Jones, Anton M. Koekemoer, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Britton Smith, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: UV β slopes as a function of UV magnitude and stellar mass (color-coded by redshift) from this work are shown as circles; all other symbols and the shaded line are the same as in Figure 5. Where our sample overlaps with previous works, our results are consistent, albeit with lower scatter. With our sample alone, we see a moderately strong correlation with stellar mass but a negligible correlation with UV magnitude. When combining our sample with previous work, we see a weak trend between the UV spectral slope and UV magnitude and a somewhat stronger trend with stellar mass, where brighter, more massive galaxies exhibit redder UV colors than faint, low-mass counterparts. The corresponding Spearman R correlation coefficients are listed for this work only in the lower right corner of each panel.
Paper: Rest-frame UV Colors for Faint Galaxies at z ∼ 9–16 with the JWST NGDEEP Survey
Authors: Alexa M. Morales, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Nikko J. Cleri, Romeel Dave, Mark Dickinson, Henry C. Ferguson, Nimish P. Hathi, Ewan Jones, Anton M. Koekemoer, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Britton Smith, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption:  BAGPIPES SEDs to observed photometry for all 36 galaxies in our sample. The solid black line is the least χ 2 SED model, the dark-gray shaded regions indicate the 1σ bounds of all 1000 SEDs fit to the photometry, while the light-gray shaded regions are the full (100th percentile) range of the SED models. The orange points are the observed photometry taken with JWST. The orange (and purple) lines and shaded regions are the median and 1σ confidence interval for the measured β PL (and β SED), as noted in the legends.
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: Normalized Q/I and U/I Stokes parameters in the 2–8 keV band. The black and green points represent the results of the third and fourth IXPE observations for 1ES 1959+650, respectively. The magenta point represents the result of the IXPE observation for PKS 2155–304.
Paper: Using JWST Transits and Occultations to Determine ∼1% Stellar Radii and Temperatures of Low-mass Stars
Authors: Alexandra S. Mahajan, Jason D. Eastman, James Kirk
Figure caption: All primary transit light curves used in our global model, plotted with an arbitrary offset. The black points represent each respective data point and the red lines represent the best-fit model using EXOFASTv2. Labels above each transit state the telescope, epoch, and filter used for the observation.
Paper: Evidence of High-latitude Emission in the Prompt Phase of GRBs: How Far from the Central Engine are the GRBs Produced?
Authors: Z. Lucas Uhm, Donggeun Tak, Bing Zhang, Judith Racusin, Daniel Kocevski, Sylvain Guiriec, Bin-Bin Zhang, Julie McEnery
Figure caption: Lightcurves and time-dependent spectra of our numerical models [u], [v], and [w]. The top panels show the lightcurves at 100 keV, 300 keV, and 1 MeV, together with the temporal evolution of E  p  curves. The middle panels show time-dependent spectra at 1, 2, and 3 s, with the curvature effect of HLE (Uhm & Zhang 2015) fully included (solid lines) or removed (dotted lines) for model [u]. The ν F  ν  spectra in the bottom panels are derived from the corresponding solid lines in the middle panels.
Paper: Evidence of High-latitude Emission in the Prompt Phase of GRBs: How Far from the Central Engine are the GRBs Produced?
Authors: Z. Lucas Uhm, Donggeun Tak, Bing Zhang, Judith Racusin, Daniel Kocevski, Sylvain Guiriec, Bin-Bin Zhang, Julie McEnery
Figure caption: Results of our time-resolved spectral analysis performed on three example broad pulses in GRB 110301A, GRB 140329A, and GRB 160113A. The top panels show the lightcurves at three different energy bands, together with the temporal evolution of E  p  points. The bottom panels show the E  p  vs. ﹩{F}_{\nu ,{E}_{p}}﹩ points obtained from the analysis. The dotted line indicates the relation ﹩{F}_{\nu ,{E}_{p}}\propto {E}_{p}^{\,2}﹩ in Equation (1). The color gradient in the bottom panels is in accordance with the color gradient encoded in the E  p  points in the top panels.
Paper: Evidence of High-latitude Emission in the Prompt Phase of GRBs: How Far from the Central Engine are the GRBs Produced?
Authors: Z. Lucas Uhm, Donggeun Tak, Bing Zhang, Judith Racusin, Daniel Kocevski, Sylvain Guiriec, Bin-Bin Zhang, Julie McEnery
Figure caption: The peak energy E  p  vs. the spectral flux F  ν  at E  p  (i.e., ﹩{F}_{\nu ,{E}_{p}}﹩) across the broad pulses of our numerical models [u], [v], and [w]. An open circle in each model marks the first point at the beginning of pulses. The dotted line indicates the relation ﹩{F}_{\nu ,{E}_{p}}\propto {E}_{p}^{\,2}﹩ in Equation (1).
Paper: Evidence of High-latitude Emission in the Prompt Phase of GRBs: How Far from the Central Engine are the GRBs Produced?
Authors: Z. Lucas Uhm, Donggeun Tak, Bing Zhang, Judith Racusin, Daniel Kocevski, Sylvain Guiriec, Bin-Bin Zhang, Julie McEnery
Figure caption: Profile of characteristic Lorentz factor γ ch of electrons in our numerical models [u], [v], and [w].
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: Polarization degree as a function of energy bin for 1ES 1959+650 and PKS 2155–304, where the polarization degrees were estimated by the software ixpeobssim. The red, blue, black, and green points represent the results of the first, second, third, and fourth IXPE observations for 1ES 1959+650, respectively. The magenta points represent the result of the IXPE observation for PKS 2155–304. If the estimated value of ΠX is smaller than MDP99, then the MDP99 value is taken as an upper limit for that energy bin and represented as an open inverted triangle.
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: The long-term light curves derived by the Fermi-LAT and Swift-XRT observations for the two HBLs. The ∼15 yr γ-ray light curves are derived with an adaptive-binning method based on a criterion of TS > 25 for each time bin, where the minimum time-bin step is 15 days. The XRT data are taken from a long-term Swift monitoring program of Fermi γ-ray sources (Stroh & Falcone 2013). In the top panel, the red, blue, black, and green horizontal lines indicate the flux states in X-ray and γ-ray bands during the first, second, third, and fourth IXPE observations for 1ES 1959+650. In the bottom panel, the magenta horizontal lines indicate the flux states in X-ray and γ-ray bands during the IXPE observation for PKS 2155–304, while the black dashed horizontal line represents the ∼15 yr average flux in the Fermi-LAT band.
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: The light curves in X-ray and γ-ray bands during the IXPE observations for the two HBLs. The X-rays are obtained by analyzing the XRT observational data. The γ-ray light curves are derived with an adaptive-binning method based on a criterion of TS > 25 for each time bin, where the minimum time-bin step is 6 hr. The two purple vertical lines represent the IXPE observation time. The top and middle panels, respectively, correspond to the third and fourth IXPE observations of 1ES 1959+650. The bottom panel indicates the result during the IXPE observation of PKS 2155–304.
Paper: Using JWST Transits and Occultations to Determine ∼1% Stellar Radii and Temperatures of Low-mass Stars
Authors: Alexandra S. Mahajan, Jason D. Eastman, James Kirk
Figure caption: The upper panel shows the primary JWST transit of GJ 1214b. The black points represent each respective data point, the red line represents the best-fit model using EXOFASTv2, and the lower panel represents the model’s residuals of observed minus calculated. The JWST light curve is available as data behind the figure.(The data used to create this figure are available.)
Paper: Using JWST Transits and Occultations to Determine ∼1% Stellar Radii and Temperatures of Low-mass Stars
Authors: Alexandra S. Mahajan, Jason D. Eastman, James Kirk
Figure caption: The upper panel shows the SED model for GJ 1214 of brightness vs. wavelength in microns. The black line represents the model’s atmosphere and the red horizontal bars represent the wavelength span of the observations in the star. The blue points represent the model and the average over the span of the width of the red horizontal bars. The red vertical bars represent the uncertainty in the measurement; the bottom panel represents the model’s residuals of observed minus calculated divided by the uncertainty.
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: ΓX against F 0.3−10 keV for PKS 2155–304, where ΓX and F 0.3−10 keV are the photon spectral index and flux in the 0.3–10 keV band and derived with the XRT observation data during the IXPE observation. Using the bootstrap method to estimate the correlation coefficient (r), we obtain r = −0.54.
Paper: X-Ray Polarization Variability of High Spectral Peak BL Lacertaes: Cases of 1ES 1959+650 and PKS 2155–304
Authors: Xin-Ke Hu, Yu-Wei Yu, Jin Zhang, Tan-Zheng Wu, Ji-Shun Lian, Xiang-Gao Wang, Hai-Ming Zhang, En-Wei Liang
Figure caption: Spectral analysis results of X-rays. The black, red, and blue points indicate the data from Swift-XRT, NuSTAR-FPMA, and NuSTAR-FPMB, respectively. The six spectra relate to the observations performed on 2022 May 3 (top left), 2022 June 12 (top right), 2022 October 31 (mid left), 2023 August 14 (mid right), 2023 August 19 (bottom left), and 2023 November 1 (bottom right), respectively.
Paper: Using JWST Transits and Occultations to Determine ∼1% Stellar Radii and Temperatures of Low-mass Stars
Authors: Alexandra S. Mahajan, Jason D. Eastman, James Kirk
Figure caption: Same as Figure 2, but for the JWST secondary eclipse. Note the transit has been normalized so that the stellar flux (i.e., during the secondary eclipse) is 1.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Example maps in the BOPS survey. First column: 870 μm dust polarization intensity in color scale overlaid with the redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), polarization segments, and dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the B-field segments (i.e., polarization rotated by 90°) and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. In the second and third panels, the black segments represent the B-fields. The red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. The gray arrows in the second and third columns indicate the mean B-field directions weighted by the intensity including all the polarization segments and weighted by the uncertainty within an annular region of 400–1000 au, respectively. In the first, second, and third columns, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed and solid circles correspond to scales of 1000 and 400 au, respectively. Fourth column: C17O PV diagram perpendicular to the outflow direction. The color scale indicates the total intensity of the C17O line. Black solid contour levels are 3 times the intensity rms × (1, 2, 4, 8, 16, 32, 64), while dashed contours are set at 3 times the intensity rms × (−1, −2, −4). Vertical dashed lines represent a scale of 400 au, with a blue line indicating a blueshifted offset of 200 au and a red line indicating a redshifted offset of 200 au. The red and blue horizontal lines indicate the velocity values corresponding to the positions with the highest intensity on the 200 au redshifted and blueshifted scales, respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Histograms of angle’s differences for the 17 protostars with compact, barely resolved polarized emission thought to be related to dust polarization caused by dust self-scattering (top panels) and for the rest of the protostars with extended polarized emission (bottom panels). Top panels: histogram of the angle difference between the outflow direction θ Out and the mean polarization direction weighted by the intensity 〈θ Pol〉 I  (left) and between the disk orientation along the major axis θ Disk and the mean polarization direction 〈θ Pol〉 I  (right). In the histogram in the top right panel, one disk, from HOPS-354, is not included because the disk is probably nearly face-on. Bottom panels: histogram of the angle difference between the outflow direction θ Out and the intensity-weighted average B-field direction using all the detected polarized emission ﹩\langle {\theta }_{{B}_{1}}{\rangle }_{I}﹩ (left) and within an annular region with inner and outer radii of 400 and 1000 au ﹩\langle {\theta }_{{B}_{2}}{\rangle }_{I}﹩ (right), respectively. HOPS-250 is not included in the bottom right panel because there is no 4σ polarization detection within the annular region.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Number of protostars for different types of B-field morphology. In the first column, green rings indicate protoplanetary envelope (disk for self-scattering), and star symbols located at the center indicate protostars. Red and blue arrows indicate the outflow directions. Black curves and segments indicate the B-field orientation, while magenta segments indicate polarization direction. HOPS-250, which does not have 4σ polarization detection within the annular region from 400 to 1000 au scale, is included in the type of Not enough data, which is marked by the asterisk.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Nonperp-Type: velocity gradient direction is not perpendicular to outflow direction (∣θ Out − θ  v ∣ < 67.°5). First column: 870 μm dust polarization intensity in color scale overlaid with the redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), polarization segments, and dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the B-field segments (i.e., polarization rotated by 90°) and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. In the second and third panels, the black segments represent the B-fields. The red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. The gray arrows in the second and third columns indicate the mean B-field directions weighted by the intensity including all the polarization segments and weighted by the uncertainty within an annular region of 400–1000 au, respectively. In all panels, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed and solid circles correspond to scales of 1000 and 400 au, respectively.