adsabs/AstroCLIMB huggingface dataset:
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Count light curves of Fermi-GBM during the time span of 0–30 s. The differently shaded regions marked with different colors denote the two independent thermally subdominated episodes: ﹩{P}_{1}^{\mathrm{th}}﹩ (pink) and ﹩{P}_{2}^{\mathrm{th}}﹩ (blue), the afterglow emission episode P AO (yellow), and the gamma-ray flare emission P 3 (gray). Left: the two horizontal dashed lines represent the limiting values of α = −2/3 and α = −3/2 for electrons in the synchrotron slow- and fast-cooling regimes, respectively. The data points that are connected by the solid orange lines represent the temporal evolution of the low-energy photon index α of the CPL-only fits. Right: the data points that are connected by the solid orange lines represent the temporal evolution of E p for the Band-only fits, while those in red indicate the temporal evolution of the E c for the CPL-only fits.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Spectrum from 4.95 to 5.45 s. The spectrum includes data from Fermi-GBM (2 Na I and 1 BGO detector). The fitting is presented by the solid line, including the components of a Planck BB function, indicated by the dashed line, and a CPL function, indicated by the dotted line.
Paper: A Cosmological Fireball with 16% Gamma-Ray Radiative Efficiency
Authors: Liang Li, Yu Wang, Felix Ryde, Asaf Pe'er, Bing Zhang, Sylvain Guiriec, Alberto J. Castro-Tirado, D. Alexander Kann, Magnus Axelsson, Kim Page, Péter Veres, P. N. Bhat
Figure caption: Bayesian MC time-integrated spectral fits for the Fermi-GBM data (from 0 s to 116 s; T 90 duration). We apply 20 chains, with each chain iterating 104 times and burning the first 103 times. The parameters are the normalization (Norm CPL), cutoff energy, and power-law index of the CPL model, as well as the normalization (Norm BB) and temperature (kT) of the BB model.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: The effect of Rosseland mean opacity (κ BL) and VSI wavelength mode (λ  x ) on the dimensionless cooling-time parameter t coolΩk. At cooling times below t critΩk the VSI can become active. An increased opacity increases the cooling time in the inner, optically thick regions of the disk and decreases the cooling time in the outer, optically thin disk regions. As a result the VSI-prone region shifts outwards in the disk.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: The evolution of the gas (dashed) and dust (solid) surface density for a selection of models from the grid of parameters explored. Each panel shows a combination of particle size and centrifugal radius. All models shown here used an initial dust-to-gas ratio of Z = 0.01. The black lines indicate the time, as labeled, at which 500 M ⊕ have piled up inside 20 au. The model selected as the best fit for IM Lup is shown in the center-right panel, with a particle size of 1 mm and a centrifugal radius of 250 au. Changing the centrifugal radius has a minor effect on the evolution of the dust, but it affects the size of the gas disk at the time of the pileup. Models with particle sizes of 3 mm only reach 500 M ⊕ of dust within 20 au just after the disk has finished forming, and would thus likely represent objects that are still embedded in their natal envelope. In the models with dust particles that are 0.2 mm in size, dust drift is too inefficient to pile up 500 M ⊕ in the inner 20 au at any time.
Paper: A Potential Site for Wide-orbit Giant Planet Formation in the IM Lup Disk
Authors: Arthur D. Bosman, Johan Appelgren, Edwin A. Bergin, Michiel Lambrechts, Anders Johansen
Figure caption: Same as Figure 4, but assuming a wavelength mode of λ x = 0.5 H g. At longer wavelengths cooling is less efficient in the optically thick regions of the disk. As a result, the inner edge of the VSI-active region moves outwards and millimeter-sized dust particles remain settled in the innermost region of the disk.
Paper: Two Lensed Star Candidates at z ≃ 4.8 behind the Galaxy Cluster MACS J0647.7+7015
Authors: Ashish Kumar Meena, Adi Zitrin, Yolanda Jiménez-Teja, Erik Zackrisson, Wenlei Chen, Dan Coe, Jose M. Diego, Paola Dimauro, Lukas J. Furtak, Patrick L. Kelly, Masamune Oguri, Brian Welch, Abdurro'uf, Felipe Andrade-Santos, Angela Adamo, Rachana Bhatawdekar, Maruša Bradač, Larry D. Bradley, Tom Broadhurst, Christopher J. Conselice, Pratika Dayal, Megan Donahue, Brenda L. Frye, Seiji Fujimoto, Tiger Yu-Yang Hsiao, Vasily Kokorev, Guillaume Mahler, Eros Vanzella, Rogier A. Windhorst
Figure caption: Radius–magnification limits for highly magnified stars. The red and blue lines represent the peak magnifications reached by microcaustic crossings as a function of the star’s radius (Venumadhav et al. 2017; Oguri et al. 2018), for the two scenarios implied by the locations of star-1 and star-2, respectively. The filled black circles along the solid and dashed black lines indicate the relation between stellar radius, for the T eff ≈ 10,000 K (star-1) and T eff ≈ 12,000 K (star-2) models of different initial mass from the BoOST (Szecsi et al. 2022) SMC-metallicity stellar evolutionary tracks, and the magnification required for these to match the apparent brightness of the two candidates. For star-1, only stellar models with initial masses ≳20 M ⊙ on the solid black line fall below the blue radius–magnification line, and are thus considered plausible, whereas stars smaller than this mass limit fall above the blue line, indicating they require too large magnifications for their predicted sizes. Similarly, for star-2 only stars with masses ≳50 M ⊙ on the dashed black line fall below the red line and remain viable candidates. In the case of the stellar evolutionary tracks used here, stars with initial masses above 100 M ⊙ never reach temperatures as low as those inferred by the SED fits to our two candidates.
Paper: Two Lensed Star Candidates at z ≃ 4.8 behind the Galaxy Cluster MACS J0647.7+7015
Authors: Ashish Kumar Meena, Adi Zitrin, Yolanda Jiménez-Teja, Erik Zackrisson, Wenlei Chen, Dan Coe, Jose M. Diego, Paola Dimauro, Lukas J. Furtak, Patrick L. Kelly, Masamune Oguri, Brian Welch, Abdurro'uf, Felipe Andrade-Santos, Angela Adamo, Rachana Bhatawdekar, Maruša Bradač, Larry D. Bradley, Tom Broadhurst, Christopher J. Conselice, Pratika Dayal, Megan Donahue, Brenda L. Frye, Seiji Fujimoto, Tiger Yu-Yang Hsiao, Vasily Kokorev, Guillaume Mahler, Eros Vanzella, Rogier A. Windhorst
Figure caption: Highly magnified star candidates in the strongly lensed arc at z  s  = 4.8. The dashed red and green curves represent the critical curve corresponding to the dPIEeNFW and Glafic lens mass models, respectively. The positions of star-1 and star-2 are marked by the green and white stars, respectively. The dashed yellow line perpendicular the arc shows the position of the macro-critical curve on the arc estimated model-independently using the distances between the counter-images of two strongly lensed knots. These knots sit at the endpoints of the white lines drawn along the arc. The blue arrows show various multiply imaged clumps in the galaxy. The yellow-circled clumps are the only one used in the dPIEeNFW lens model reconstruction. The white circle marks the position of a fainter, possible counter-image of star-2. The panel is 8.″4 × 8.″4 across.
Paper: Two Lensed Star Candidates at z ≃ 4.8 behind the Galaxy Cluster MACS J0647.7+7015
Authors: Ashish Kumar Meena, Adi Zitrin, Yolanda Jiménez-Teja, Erik Zackrisson, Wenlei Chen, Dan Coe, Jose M. Diego, Paola Dimauro, Lukas J. Furtak, Patrick L. Kelly, Masamune Oguri, Brian Welch, Abdurro'uf, Felipe Andrade-Santos, Angela Adamo, Rachana Bhatawdekar, Maruša Bradač, Larry D. Bradley, Tom Broadhurst, Christopher J. Conselice, Pratika Dayal, Megan Donahue, Brenda L. Frye, Seiji Fujimoto, Tiger Yu-Yang Hsiao, Vasily Kokorev, Guillaume Mahler, Eros Vanzella, Rogier A. Windhorst
Figure caption: Measured photometry of star-1 and star-2 and the corresponding SED model fits are shown in middle and bottom panels, respectively. The black solid points with error bars represent the observed AB magnitudes and their 1σ errors, respectively, for the lensed star candidates, in the various JWST/NIRCam filters. The red, green, and blue curves for each candidate represent three acceptable single-star SED fits, with the green SED being the best-fitting one. For the green SEDs, we also plot the integrated broadband fluxes (filled squares) resulting from the model and present the best-fitting ﹩\mathrm{log}(\mu L/{L}_{\odot })﹩ scaling of this fit. The filter throughput curves are shown on the top panel.
Paper: Two Lensed Star Candidates at z ≃ 4.8 behind the Galaxy Cluster MACS J0647.7+7015
Authors: Ashish Kumar Meena, Adi Zitrin, Yolanda Jiménez-Teja, Erik Zackrisson, Wenlei Chen, Dan Coe, Jose M. Diego, Paola Dimauro, Lukas J. Furtak, Patrick L. Kelly, Masamune Oguri, Brian Welch, Abdurro'uf, Felipe Andrade-Santos, Angela Adamo, Rachana Bhatawdekar, Maruša Bradač, Larry D. Bradley, Tom Broadhurst, Christopher J. Conselice, Pratika Dayal, Megan Donahue, Brenda L. Frye, Seiji Fujimoto, Tiger Yu-Yang Hsiao, Vasily Kokorev, Guillaume Mahler, Eros Vanzella, Rogier A. Windhorst
Figure caption: The two lensed star candidates in different JWST filters. In each panel, the positions of star-1 and star-2 on the lensed arc are shown by green and red arrows, respectively. Each panel is 8.″4 × 8.″4 across.
Paper: A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910
Authors: Silvia Zane, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, Mason Ng, Toru Tamagawa, Ilaria Caiazzo, Niccolò Di Lalla, Herman L. Marshall, Matteo Bachetti, Fabio La Monaca, Ephraim Gau, Alessandro Di Marco, Luca Baldini, Michela Negro, Nicola Omodei, John Rankin, Giorgio Matt, George G. Pavlov, Takao Kitaguchi, Henric Krawczynski, Fabian Kislat, Ruth Kelly, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: 1RXS J1708 IXPE observation (blue circles with error bars) for the source counts (panels (A)–(C)) and polarization degree (panels (D)–(F)), plotted as a function of the rotational phase (in each row, the three panels from the left to the right show the data integrated over the 2–8, 2–4, and 4–8 keV bands, respectively). Panels (G) and (H) show: (left) the phase averaged spectrum (solid lines) together with the contributions of the condensed zone (dashed lines) and atmospheric zone (dotted lines); (right) the polarization angle as a function of the rotational phase, integrated over the 2–8 keV band. Errors are shown at the 1σ level assuming the polarization degree and polarization angle are not correlated. In all panels, the orange and green lines represent the model expectation within the belt+cap and cap+cap scenarios (solid lines for the total model, dotted and dashed lines in panel (G) only for the two separate components); the red solid line in panel (H) shows the RVM (see the text for the parameter values and other details). Note that data points in the phase-resolved analysis are obtained with IXPEOBSSIM, and therefore independent on the spectral decomposition.
Paper: A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910
Authors: Silvia Zane, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, Mason Ng, Toru Tamagawa, Ilaria Caiazzo, Niccolò Di Lalla, Herman L. Marshall, Matteo Bachetti, Fabio La Monaca, Ephraim Gau, Alessandro Di Marco, Luca Baldini, Michela Negro, Nicola Omodei, John Rankin, Giorgio Matt, George G. Pavlov, Takao Kitaguchi, Henric Krawczynski, Fabian Kislat, Ruth Kelly, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Left: phase- and energy-averaged linear polarization of 1RXS J1708, in terms of the normalized Stokes parameters. Uncertainties are shown at the 68.3% (1σ) confidence level. Circles with center in the origin and increasing radii correspond to increasing values of the polarization degree while different values of the azimuth to different polarization angles. Right: polarization of 1RXS J1708 in different energy bands, computed with IXPEOBSSIM. Contours identify the 50% confidence regions for the joint measurement of the polarization degree and angle (which are not independent variables), accounting for statistical fluctuations only. Orange stars and green crosses show, for the same energy bins, the prediction of the belt+cap and cap+cap models, respectively (see Section 5 for details).
Paper: A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910
Authors: Silvia Zane, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, Mason Ng, Toru Tamagawa, Ilaria Caiazzo, Niccolò Di Lalla, Herman L. Marshall, Matteo Bachetti, Fabio La Monaca, Ephraim Gau, Alessandro Di Marco, Luca Baldini, Michela Negro, Nicola Omodei, John Rankin, Giorgio Matt, George G. Pavlov, Takao Kitaguchi, Henric Krawczynski, Fabian Kislat, Ruth Kelly, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Joint spectropolarimetric fit of IXPE, Swift/XRT, and NICER data. The Stokes I, Q, and U energy spectra are obtained by binning the event-by-event Stokes parameters, calculated following Kislat et al. (2015), according to the measured energy of the event. Q and U are given by the source flux multiplied by the polarization degree and either the cosine or the sine of twice the polarization angle, respectively. The Stokes I, Q, and U energy spectra convolved with the instrument response are shown in the left, central, and right panels, respectively. The best-fit model of the form TBABS*(BBODY * POLCONST + POWERLAW * POLCONST) is shown by the solid lines. Fit residuals are shown in the bottom panels; see Table 2 in Appendix B for the fit parameters. Light colored curves are the background of IXPE detectors.
Paper: A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910
Authors: Silvia Zane, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, Mason Ng, Toru Tamagawa, Ilaria Caiazzo, Niccolò Di Lalla, Herman L. Marshall, Matteo Bachetti, Fabio La Monaca, Ephraim Gau, Alessandro Di Marco, Luca Baldini, Michela Negro, Nicola Omodei, John Rankin, Giorgio Matt, George G. Pavlov, Takao Kitaguchi, Henric Krawczynski, Fabian Kislat, Ruth Kelly, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Top panel: 1RXS J1708 lightcurve, averaged over the three IXPE telescopes, for the source and the background. The count rate is averaged over 500 s and integrated over the IXPE nominal energy band, 2.0–8.0 keV. Middle and bottom panels: lightcurve of normalized Stokes parameters; the time bin is 20 ks. In all panels, variations are compatible with statistical fluctuations only: the null probabilty for a fit with a constant is acceptable.
Paper: A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910
Authors: Silvia Zane, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, Mason Ng, Toru Tamagawa, Ilaria Caiazzo, Niccolò Di Lalla, Herman L. Marshall, Matteo Bachetti, Fabio La Monaca, Ephraim Gau, Alessandro Di Marco, Luca Baldini, Michela Negro, Nicola Omodei, John Rankin, Giorgio Matt, George G. Pavlov, Takao Kitaguchi, Henric Krawczynski, Fabian Kislat, Ruth Kelly, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Same as in Figure 2, for the TBABS*(BBODY * POLCONST + BBODY * POLCONST) model. See Table 2 in Appendix B for the fit parameters.
Paper: Early Stages of Galilean Moon Formation in a Water-depleted Environment
Authors: Olivier Mousis, A. Schneeberger, Jonathan I. Lunine, Christopher R. Glein, Alexis Bouquet, Steven D. Vance
Figure caption: Temperature, surface density, and pressure profiles in the CPD expressed in units of Jovian radii (R Jup), and calculated at t = 104, 105, and 106 yr. The vertical bars designated by the letters I, E, G, and C correspond to the current orbits of Io, Europa, Ganymede, and Callisto, respectively. The vertical brown and blue rectangles correspond to the time evolution of the PDL and SL over 106 yr in the CPD, respectively. A phyllosilicate dehydration temperature of 500 K is assumed in the figure.
Paper: Early Stages of Galilean Moon Formation in a Water-depleted Environment
Authors: Olivier Mousis, A. Schneeberger, Jonathan I. Lunine, Christopher R. Glein, Alexis Bouquet, Steven D. Vance
Figure caption: Radial profile of the water abundance within the Jovian CPD expressed as a function of the initial abundance in phyllosilicates, assuming its vapor form is sourced by the dehydration of phyllosilicate-rich particles during their inward drift, and calculated at t = 104, 105, and 106 yr. Three dehydration temperatures are considered: 600 K (top row), 500 K (middle row), and 400 K (bottom row). The horizontal dashed line denotes the threshold at which the amount of condensed water is sufficient to account for that in Ganymede and Callisto. The brown and blue vertical dashed lines correspond to the locations of the PDL and SL in the CPD, respectively.