adsabs/AstroCLIMB huggingface dataset:
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, 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, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Energy distributions of the Stokes parameters I, Q, and U for the bright state of Cen X-3 superimposed to the best-fit model (top panels). The residuals between data and model normalized for the errors are shown in the bottom panels. The different colors represent the three IXPE detectors: DU1 in blue, DU2 in orange, and DU3 in green.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, 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, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Dependence of the normalized flux, normalized Stokes parameters q and u on the pulse phase in the 2–8 keV energy band in the bright state of Cen X-3 estimated using the formalism of Kislat et al. (2015). Data from the three IXPE telescopes are combined.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, 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, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Polarization vector of Cen X-3 based on the spectral fitting of the pulse phase-averaged data collected in the bright state. The PD and PA confidence level contours at 1σ, 2σ, and 3σ are presented in polar coordinates in red, green, and blue, respectively. The PA is measured from north to east as seen by the observer.
Paper: The X-Ray Polarimetry View of the Accreting Pulsar Cen X-3
Authors: Sergey S. Tsygankov, Victor Doroshenko, Juri Poutanen, Jeremy Heyl, Alexander A. Mushtukov, Ilaria Caiazzo, Alessandro Di Marco, Sofia V. Forsblom, Denis González-Caniulef, Moritz Klawin, Fabio La Monaca, Christian Malacaria, Herman L. Marshall, Fabio Muleri, Mason Ng, Valery F. Suleimanov, Rashid A. Sunyaev, Roberto Turolla, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, 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, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Pulse profile of Cen X-3 in different energy bands as seen by IXPE in the low (orange) and bright (blue) states. Data from the three telescopes were combined.
Paper: Evidence of a Nonorthogonal X-line in Guide-field Magnetic Reconnection
Authors: Neha Pathak, R. E. Ergun, Y. Qi, S. J. Schwartz, T. Vo, M. E. Usanova, M. Hesse, T. D. Phan, J. F. Drake, S. Eriksson, N. Ahmadi, A. Chasapis, F. D. Wilder, J. E. Stawarz, J. L. Burch, K. J. Genestreti, R. B. Torbert, R. Nakamura
Figure caption: (a)–(c) B  L , B  M , and B  N  from all of the MMS spacecraft. (d) The Hall electric field (E  N ) for each spacecraft. (e)–(f) The electron jet V  L  and the electron current V  M .The electron jet reversal for MMS1 and MMS2 is at the same time as the current sheet crossing. (g) The relative positions of all the MMS spacecraft. (h) Relevant plasma parameters.
Paper: Evidence of a Nonorthogonal X-line in Guide-field Magnetic Reconnection
Authors: Neha Pathak, R. E. Ergun, Y. Qi, S. J. Schwartz, T. Vo, M. E. Usanova, M. Hesse, T. D. Phan, J. F. Drake, S. Eriksson, N. Ahmadi, A. Chasapis, F. D. Wilder, J. E. Stawarz, J. L. Burch, K. J. Genestreti, R. B. Torbert, R. Nakamura
Figure caption: (a) The directional derivatives of  B  in a hemisphere looking from GSE-Y. White contours highlight the minimum and maximum directional derivatives. The maximum directional derivative is within few degrees of variance-determined N. The minimum directional derivative (M′) is 60° from variance-determined M and is nearly along the MMS1–MMS2 direction. (b) A cartoon showing that a nonorthogonal X-line sets MMS1 and MMS2 simultaneously at the X-line in the EDR. Because of the shear in the L–N planes, motion in the M-direction leads to apparent motion in the L-direction. The directional derivatives of (c) B  M  and (d) E  N .
Paper: Evidence of a Nonorthogonal X-line in Guide-field Magnetic Reconnection
Authors: Neha Pathak, R. E. Ergun, Y. Qi, S. J. Schwartz, T. Vo, M. E. Usanova, M. Hesse, T. D. Phan, J. F. Drake, S. Eriksson, N. Ahmadi, A. Chasapis, F. D. Wilder, J. E. Stawarz, J. L. Burch, K. J. Genestreti, R. B. Torbert, R. Nakamura
Figure caption: ((a)–(d)) Measured values of B  L , J  M , J  L , and E  N  along their estimated paths through the EDR using the nonorthogonal model. The gold area represents the EDR. The MMS1 path is offset 2 km in N, and the MMS2 path is offset −2 km in N so that both can be seen. The MMS1 and MMS2 traces are half the width of the other traces. (e) A zoomed-in view of J  L  along the MMS paths. MMS1, MMS2, and MMS3 show the jet reversal at nearly the same position under the nonorthogonal model. (f) The jet reversal is misaligned using a model with physical motion in L.
Paper: First Wide Field-of-view X-Ray Observations by a Lobster-eye Focusing Telescope in Orbit
Authors: C. Zhang, Z. X. Ling, X. J. Sun, S. L. Sun, Y. Liu, Z. D. Li, Y. L. Xue, Y. F. Chen, Y. F. Dai, Z. Q. Jia, H. Y. Liu, X. F. Zhang, Y. H. Zhang, S. N. Zhang, F. S. Chen, Z. W. Cheng, W. Fu, Y. X. Han, H. Li, J. F. Li, Y. Li, P. R. Liu, X. H. Ma, Y. J. Tang, C. B. Wang, R. J. Xie, A. L. Yan, Q. Zhang, B. W. Jiang, G. Jin, L. H. Li, X. B. Qiu, D. T. Su, J. N. Sun, Z. Xu, S. K. Zhang, Z. Zhang, N. Zhang, X. Z. Bi, Z. M. Cai, J. W. He, H. Q. Liu, X. C. Zhu, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, C. C. Jin, D. Y. Li, H. W. Pan, W. X. Wang, Y. F. Xu, X. Yang, B. Zhang, M. Zhang, W. D. Zhang, D. H. Zhao, M. Bai, Z. Ji, Y. R. Liu, F. L. Ma, J. Su, J. Z. Tong, Y. S. Wang, Z. J. Zhao, C. Feldman, P. O'Brien, J. P. Osborne, R. Willingale, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt, E. Kuulkers, W. Yuan
Figure caption: Upper left: image of a pointlike source (PSF) with an X-ray continuum spectrum peaking at 2.5 keV seen at the center of a quadrant of the FoV obtained at XIB/NAOC (on a logarithmic color scale). Note that the image distance was adjusted accordingly for the finite X-ray source distance. Upper right: a mosaic of images of the PSF obtained at 1.25 keV in 11 × 11 directions across a quadrant of the FoV, taken with the complete module at IHEP/100XF. Lower left: positional deviations of the PSF centers from the source directions on the detector plane measured for a quadrant of the mirror assembly at NAOC/XIB. The maximum deviation is 1.′1. Lower right: a typical effective area curve of the mirror assembly for the central focal spot vs. photon energy measured at MPE/PANTER and comparison with the simulation.
Paper: First Wide Field-of-view X-Ray Observations by a Lobster-eye Focusing Telescope in Orbit
Authors: C. Zhang, Z. X. Ling, X. J. Sun, S. L. Sun, Y. Liu, Z. D. Li, Y. L. Xue, Y. F. Chen, Y. F. Dai, Z. Q. Jia, H. Y. Liu, X. F. Zhang, Y. H. Zhang, S. N. Zhang, F. S. Chen, Z. W. Cheng, W. Fu, Y. X. Han, H. Li, J. F. Li, Y. Li, P. R. Liu, X. H. Ma, Y. J. Tang, C. B. Wang, R. J. Xie, A. L. Yan, Q. Zhang, B. W. Jiang, G. Jin, L. H. Li, X. B. Qiu, D. T. Su, J. N. Sun, Z. Xu, S. K. Zhang, Z. Zhang, N. Zhang, X. Z. Bi, Z. M. Cai, J. W. He, H. Q. Liu, X. C. Zhu, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, C. C. Jin, D. Y. Li, H. W. Pan, W. X. Wang, Y. F. Xu, X. Yang, B. Zhang, M. Zhang, W. D. Zhang, D. H. Zhao, M. Bai, Z. Ji, Y. R. Liu, F. L. Ma, J. Su, J. Z. Tong, Y. S. Wang, Z. J. Zhao, C. Feldman, P. O'Brien, J. P. Osborne, R. Willingale, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt, E. Kuulkers, W. Yuan
Figure caption: Left: illustration of the configuration of the focusing mirror system, focal detector array, and FoV of LEIA. The mirror assembly is divided into four individual quadrants, each consisting of 3 × 3 MPO plates and associated with one of the four detectors. The overall FoV of the telescope module is 18.°6 × 18.°6. Right: a picture of the LEIA instrument undergoing on-ground X-ray calibration at IHEP before being assembled onto the SATech satellite.
Paper: Revisiting the Space Weather Environment of Proxima Centauri b
Authors: Cecilia Garraffo, Julián D. Alvarado-Gómez, Ofer Cohen, Jeremy J. Drake
Figure caption: Three-dimensional stellar wind simulations of Proxima Centauri driven by the observed ZDI magnetogram (left), the proxy magnetogram (middle), and the synthetic dynamo-generated magnetogram (right). The equatorial plane is colored according to dynamic wind pressure normalized to the solar wind pressure at 1 au. The simulated orbits for Proxima b are in white (the thick line is the circular orbit). The gray shaded surface denotes the Alfvén surface. The colored domain has a radius of 110R ⋆ (16.9R ⊙).
Paper: First Wide Field-of-view X-Ray Observations by a Lobster-eye Focusing Telescope in Orbit
Authors: C. Zhang, Z. X. Ling, X. J. Sun, S. L. Sun, Y. Liu, Z. D. Li, Y. L. Xue, Y. F. Chen, Y. F. Dai, Z. Q. Jia, H. Y. Liu, X. F. Zhang, Y. H. Zhang, S. N. Zhang, F. S. Chen, Z. W. Cheng, W. Fu, Y. X. Han, H. Li, J. F. Li, Y. Li, P. R. Liu, X. H. Ma, Y. J. Tang, C. B. Wang, R. J. Xie, A. L. Yan, Q. Zhang, B. W. Jiang, G. Jin, L. H. Li, X. B. Qiu, D. T. Su, J. N. Sun, Z. Xu, S. K. Zhang, Z. Zhang, N. Zhang, X. Z. Bi, Z. M. Cai, J. W. He, H. Q. Liu, X. C. Zhu, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, C. C. Jin, D. Y. Li, H. W. Pan, W. X. Wang, Y. F. Xu, X. Yang, B. Zhang, M. Zhang, W. D. Zhang, D. H. Zhao, M. Bai, Z. Ji, Y. R. Liu, F. L. Ma, J. Su, J. Z. Tong, Y. S. Wang, Z. J. Zhao, C. Feldman, P. O'Brien, J. P. Osborne, R. Willingale, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt, E. Kuulkers, W. Yuan
Figure caption: First-light X-ray image of the Galactic center region obtained by LEIA in a one-shot observation of 798 s in 0.5–4 keV, covering a field of view of 18.°6 × 18.°6 (left). The simulated observation of the same patch of sky is also shown for comparison (right). The observation identifies a source (4U 1826-24) that had become obviously much brighter than viewed at a previous observation. Colors represent counts per pixel.
Paper: Revisiting the Space Weather Environment of Proxima Centauri b
Authors: Cecilia Garraffo, Julián D. Alvarado-Gómez, Ofer Cohen, Jeremy J. Drake
Figure caption: Top: dynamic wind pressure normalized to the solar wind pressure at Earth using the proxy map (purple), the Proxima Centauri observed map (red), and the dynamo map (orange). Bottom: magnetospheric standoff distance for the same cases.
Paper: First Wide Field-of-view X-Ray Observations by a Lobster-eye Focusing Telescope in Orbit
Authors: C. Zhang, Z. X. Ling, X. J. Sun, S. L. Sun, Y. Liu, Z. D. Li, Y. L. Xue, Y. F. Chen, Y. F. Dai, Z. Q. Jia, H. Y. Liu, X. F. Zhang, Y. H. Zhang, S. N. Zhang, F. S. Chen, Z. W. Cheng, W. Fu, Y. X. Han, H. Li, J. F. Li, Y. Li, P. R. Liu, X. H. Ma, Y. J. Tang, C. B. Wang, R. J. Xie, A. L. Yan, Q. Zhang, B. W. Jiang, G. Jin, L. H. Li, X. B. Qiu, D. T. Su, J. N. Sun, Z. Xu, S. K. Zhang, Z. Zhang, N. Zhang, X. Z. Bi, Z. M. Cai, J. W. He, H. Q. Liu, X. C. Zhu, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, C. C. Jin, D. Y. Li, H. W. Pan, W. X. Wang, Y. F. Xu, X. Yang, B. Zhang, M. Zhang, W. D. Zhang, D. H. Zhao, M. Bai, Z. Ji, Y. R. Liu, F. L. Ma, J. Su, J. Z. Tong, Y. S. Wang, Z. J. Zhao, C. Feldman, P. O'Brien, J. P. Osborne, R. Willingale, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt, E. Kuulkers, W. Yuan
Figure caption: Left: X-ray image of Sco X-1 in 0.5–4 keV observed by LEIA with 673 s exposure, in excellent agreement with the PSF measured in on-ground calibration. Right: X-ray image of the Cygnus Loop nebula with a diameter of ∼2.°5 obtained with a 604 s observation (colors represent photon energies). The inset shows the PSF measured from the observation of Sco X-1 (left).
Paper: Revisiting the Space Weather Environment of Proxima Centauri b
Authors: Cecilia Garraffo, Julián D. Alvarado-Gómez, Ofer Cohen, Jeremy J. Drake
Figure caption: The different Proxima magnetograms used in this study. From top to bottom: the observed ZDI magnetogram from Klein et al. (2021), the proxy magnetogram for Proxima Cen from Garraffo et al. (2016a), and the synthetic magnetogram from the dynamo simulations of Yadav et al. (2016).
Paper: On the Injection Scale of the Turbulence in the Partially Ionized Very Local Interstellar Medium
Authors: Siyao Xu, 思遥 徐, Hui Li, 晖 李
Figure caption: The data for the magnetic energy spectrum are taken from Lee & Lee (2020) (black) and Burlaga et al. (2018) (red and blue). The dashed line indicates the Kolmogorov slope. The vertical dashed and dashed–dotted lines correspond to the damping scales of interstellar turbulence (l dam,NV,⊥; Equation (4)) and interstellar magnetic fluctuations (l dam,IN,⊥,sub−v; Equation (22)). The vertical solid line corresponds to the largest possible perpendicular injection scale (﹩{L}_{\perp ,\max }﹩; Equation (19)) of the locally driven sub-Alfvénic turbulence in the VLISM.
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The HI properties of star-forming galaxies at z ≈ 1, as a function of their stellar masses. The red circles in panels (A) and (B) show, respectively, our measurements of the average H I mass, 〈M HI〉, and the characteristic HI depletion timescale, 〈t dep,HI〉 = 〈M HI〉/〈SFR〉, for star-forming galaxies at z ≈ 1 in the three stellar-mass subsamples of Figure 2. The blue squares indicate the same quantities for the blue xGASS galaxies in three M * subsamples with stellar-mass distributions identical to those of the three subsamples at z ≈ 1. The M HI–M * relation at z ≈ 1, derived by fitting a power-law relation to our measurements of the average HI mass in the three stellar-mass subsamples, is shown as the green line in (A), with the green shaded region showing the 1σ error on the relation. Panel (A) also shows the M HI–M * relation for blue galaxies at z ≈ 0 (orange line), obtained by fitting a power-law relation to the average HI mass of xGASS galaxies in the three M * subsamples. In panel (B), the green curve shows the t dep,HI–M * relation at z ≈ 1, derived by combining our estimate of the M HI–M * relation at z ≈ 1 with the equation describing the star-forming main sequence at z ≈ 1 (Whitaker et al. 2014); the green shaded region shows the 1σ error on the relation. The orange line in (B) shows an estimate of the t dep,HI–M * relation at z ≈ 0 derived in a similar manner, by combining the M HI–M * relation at z ≈ 0 with the equation describing the star-forming main sequence at z ≈ 0 (Whitaker et al. 2012). The figure shows that blue star-forming galaxies at z ≈ 1, with stellar masses in the range M * ≈ 109–2.4×1011 M ⊙, have ≈3–4 times more HI than blue galaxies at z ≈ 0, but have far lower characteristic depletion timescales, by a factor of ≈2–4.
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The average HI 21 cm emission signal and the average rest-frame 1.4 GHz continuum emission from star-forming galaxies in the three stellar-mass subsamples. Panels (A) show the average HI 21 cm emission images of galaxies of the three stellar-mass subsamples. The HI 21 cm subcubes of each subsample were assigned weights such that their effective redshift distributions are identical. The circle on the bottom left of each panel indicates the 90 kpc spatial resolution of the images. The contour levels are at −3.0σ (dashed), +3.0σ, and +4.0σ significance. Panels (B) show the average HI 21 cm emission spectra of the three stellar-mass subsamples. The ±1σ errors on the stacked HI 21 cm spectra are indicated by the dashed black curves. We clearly detect the stacked HI 21 cm emission signals in all three subsamples. Panels (C) show the average rest-frame 1.4 GHz luminosity density images of the galaxies in the three stellar-mass subsamples. The contour levels are at 5σ, 10σ, 20σ, 40σ, and 80σ statistical significance. The circle at the bottom left of each panel indicates the 40 kpc resolution of the images.
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The characteristic HI fractions of star-forming galaxies at z ≈ 1, as a function of their sSFRs. The red circles show our measurements of the characteristic HI fraction, 〈M HI〉/〈M *〉, of star-forming galaxies at z ≈ 1 in the three sSFR subsamples of Figure 5. The black squares indicate the characteristic HI fractions of blue xGASS galaxies at z ≈ 0 in multiple sSFR bins. The dashed lines show the loci of constant gas depletion timescales. The relation between the HI fraction and the sSFR shows clear evolution from z ≈ 1 to z ≈ 0, with blue galaxies at z ≈ 0 having a characteristic HI depletion timescale of ≈4.5 Gyr (see also Saintonge et al. 2017) but those at z ≈ 1 having an HI depletion timescale of just ≈1.5 Gyr.
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The average HI 21 cm emission signals from star-forming galaxies in the three sSFR subsamples. Panels (A) show the average HI 21 cm emission images of the three sSFR mass subsamples. The circle on the bottom left of each panel indicates the 90 kpc spatial resolution of the images. The contour levels are at −3.0σ (dashed), +3.0σ, and +4.0σ significance. Panels (B) show the average HI 21 cm emission spectra of the same galaxies in the three sSFR subsamples. The ±1σ errors on the stacked HI 21 cm spectra are indicated with dashed black curves. We clearly detect the stacked HI 21 cm emission signals in all three subsamples. The HI 21 cm subcubes of each subsample were assigned weights such that their effective redshift distributions are identical.