adsabs/AstroCLIMB huggingface dataset:
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: For each telescope pair, the normalized visibility is shown as a function of local hour angle. Colored curves represent the best fit with a uniform ellipse model, and gray curves represent the best fit with a uniform disk model. The singular T1T4 data point is shown as a red square, because it passes all quality cuts, yet we suspect it may be a fit to random background fluctuations, like those discussed in Section 3.6. It is included in the fit shown. Fits are reported with and without this point in Table 2.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: The OPD-corrected projection of the correlation function as a function of relative time, defined in Equation (3). The correlation is quantified by the integral of a Gaussian peak fitted near relative time ≈ 0. This correlation function is from pair T2T3, taken at 02:31 on 2024 February 19 UTC. Before further analysis, the uncertainty on the area of the Gaussian fit (A) is replaced as discussed in Section 3.5.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: An example of a tracking correction in T2. A large negative analog-to-digital converter (ADC) value corresponds to intense light incident on the PMT. Due to tracking limitations of the array, at about 200 s into the run, the star’s image becomes slightly less centered on the PMT. At 400 s into the run, the operator adjusted the tracking, causing the telescope to briefly stop tracking the star altogether, and the current drops sharply. When the tracking is corrected, the current is stronger. The frames around the spike are removed from the correlogram before processing further.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: The correlation function as a function of relative time and time in run, for a typical 2 hr run. While the correlogram is constructed every 2 s, the vertical axis has been binned more coarsely in this figure to reduce statistical noise and make the correlation more visible. The diagonal feature is the correlation peak proportional to the squared visibility that changes during the run due to the variation in the OPD between the two telescopes. This correlation function is from pair T2T4, taken at 03:37 on 2023 December 26 UTC.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: A portion of the power spectrum for T1, as a function of frequency and time in run. Short, sporadic bursts from the on-site radio repeater produce strong signals at 79.4 MHz (an alias of the 171 MHz radio signal). Frames containing these bursts are removed from the correlogram before further processing.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: Distribution of areas from fits to background noise in the region of relative time far from the peak, for all runs. The gray band in Figure 7 corresponds to the red lines at ±3.58 fs, which are ±2σ from the mean of this distribution. This measures the spread of areas that may be found when fitting to background noise alone and includes 95% of the data in the distribution.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: Baseline coverage of the six telescope pairs in the u–v plane for the data tabulated in Table B1. Points reflect the weighted-mean position of each ∼hour-long run. The curves are point reflected about the origin and travel clockwise with time.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: A comparison of two Roche–von Zeipel synthetic spectral energy distributions (SEDs) to archival absolute spectrophotometry of γ Cas between 1200 and 8170 Å. Data for wavelengths beyond 3200 Å are from V. I. Burnashev (1996). International Ultraviolet Explorer (IUE) data have been rebinned from high dispersion to low dispersion (R. González-Riestra et al. 2000) and extracted from the IUE Newly Extracted Spectra (INES) data archive (https://sdc.cab.inta-csic.es/ines/index2.html), explicitly SWP09130RL.FITS (http://sdc.cab.inta-csic.es/ines/jsp/SingleDownload.jsp?filename=SWP09130RL.FITS) and LWR07861RL.FITS (http://sdc.cab.inta-csic.es/ines/jsp/SingleDownload.jsp?filename=LWR07861RL.FITS). The faster spinning model (Ω/Ωc = 0.9999) is more gravity darkened and requires a larger polar temperature at the same equatorial angular diameter to match the spectrophotometry.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: The uniform-disk radius from fitting A vs. baseline to data points in different slices in the u–v plane (see Figure 8), as a function of the average angle of the slice.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: Best-fit parameter distributions for the Roche–von Zeipel stellar model from fitting 1000 bootstrap samples with replacement from Table B1. The dashed lines show the 1σ lower bound error and the 1σ upper bound of each parameter: θeq, the equatorial angular diameter; Ω/Ωc, the fraction of the critical angular rotation rate; ϕ*, the position angle of the visible rotation axis; and CRvZ, the proportionality constant between the model squared visibilities and measured correlation peak integrals, which is analogous to CUD and Cnorm in Equations (4) and (6), respectively.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: A normalized high-resolution spectrum of γ Cas in the VSII bandpass from the ELODIE archive (J. Moultaka et al. 2004; observation 20030816/0030, in black) and a normalized model spectrum (in blue) from the same model Roche–von Zeipel that best fits the VERITAS data in Table B1. The rotationally broadened Hδ line at 4100 Å is filled in the emission from the disk surrounding γ Cas. The disk is not included in our model.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: A distribution of the difference between the original known area of the simulated peaks and the areas found by the fitting algorithm once they are inserted into the background noise, for many fits. The root mean square of this distribution is the uncertainty on the peak.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: A synthetic photosphere for γ Cas with θeq = 0.60 mas, Ω/Ωcrit = 0.9888, and ϕ* = 114° consistent with the best-fit values to the VERITAS interferometry. The position angle of the visible rotation pole is ambiguous by 180° without interferometric phase information; thus, the data are also consistent with ϕ* = 294°.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: An example of one simulated peak inserted into the background noise and fitted with a Gaussian function to extract its area.
Paper: Measurement of the Photosphere Oblateness of γ Cassiopeiae via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: A. Archer, J. P. Aufdenberg, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, N. B. Y. Chin, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Escobar Godoy, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, N. Korzoun, T. LeBohec, M. A. Lisa, M. Lundy, G. Maier, N. Matthews, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. G. Rose, I. Sadeh, L. Saha, M. Santander, J. Scott, G. H. Sembroski, R. Shang, D. Tak, J. V. Tucci, J. Valverde, V. V. Vassiliev, D. A. Williams, S. L. Wong
Figure caption: Using the same data shown in Figure 9, the best fit using a Roche–von Zeipel model for a rapidly rotating star.
Paper: The GHOSDT Simulations. II. Missing H2 in Simulations of a Self-regulated Interstellar Medium
Authors: Alon Gurman, Chia-Yu Hu, 家瑜 胡, Michael Y. Grudić, Ulrich P. Steinwandel, Amiel Sternberg
Figure caption: (a–e) The H2-to-H I mass ratio Rmol as a function of time for different simulation groups. (a) Resolution study. (b) Effect of magnetic fields. (c, d) Variations to feedback and simulations setup. (e) Effects of our clumping subgrid model. (f) Time-averaged values of Rmol for all simulations. The vertical dashed line and shaded region show the observed median and interquartile range for PHANGS-ALMA pixels with ΣH,tot = 10 and Σ⋆ = 40  M⊙ pc−2. Numbers indicate Rmol in % for each model.
Paper: The GHOSDT Simulations. II. Missing H2 in Simulations of a Self-regulated Interstellar Medium
Authors: Alon Gurman, Chia-Yu Hu, 家瑜 胡, Michael Y. Grudić, Ulrich P. Steinwandel, Amiel Sternberg
Figure caption: Observational data from the PHANGS-ALMA survey (A. K. Leroy et al. 2021a, 2021b; J. Sun et al. 2022). Top panel: Rmol as a function of total hydrogen surface density. Middle panel: Rmol as a function of gas weight. Bottom panel: Rmol as a function of stellar mass surface density for data with ﹩{\mathrm{log}}\left({{\rm{\Sigma }}}_{{\rm{H}},{\rm{tot}}}\right./\left({M}_{\odot }\,{{\rm{pc}}}^{-2}\right))=1\pm 0.1﹩. In all panels, the white line shows the median and the red shaded region shows the 25%–75% range. The orange lines indicate the intersection of the median and interquartile range with the solar neighborhood value of Σ⋆ = 40 M⊙ pc−2.
Paper: Multilayered Fast Wind Observed in XMM-Newton Snapshot of Seyfert 1 Markarian 877
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, W. N. Brandt, Luigi Gallo, Doyee Byun, Elena Gallo
Figure caption: The values of best-fit column densities (NH), line-of-sight outflow velocities (vz), turbulence velocities (σv), and the covering factors (fcov) of the wind as a function of best-fit ionization parameter ξ. The best-fit line between column density and ionization parameter is shown in the top panel, with shaded regions indicating the 1σ confidence level. m and α are the best slope and the associated density profile index with its 1σ uncertainty.
Paper: Multilayered Fast Wind Observed in XMM-Newton Snapshot of Seyfert 1 Markarian 877
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, W. N. Brandt, Luigi Gallo, Doyee Byun, Elena Gallo
Figure caption: Left: XMM-Newton/PN 18 ks snapshot of Mrk 877 in the source frame, fit with a simple power law. The strong flux deficits between 0.7–1.4 kev and 6.4–8.4 keV indicate multiple ionized partially covering absorption components. Right: best-fit model using three distinct UFO components with the pion photoionization model in SPEX. The green, magenta, and blue curves represent absorption from low- to high-ionization zones. These components are detected at 5σ, 4σ, and >10σ. The red curve shows the total best-fit model.
Paper: The GHOSDT Simulations. II. Missing H2 in Simulations of a Self-regulated Interstellar Medium
Authors: Alon Gurman, Chia-Yu Hu, 家瑜 胡, Michael Y. Grudić, Ulrich P. Steinwandel, Amiel Sternberg
Figure caption: Top panel: vturb as a function of density for models m100, m10, m1, and m0.25. Dashed colored lines show the corresponding solid curves scaled by ﹩{\left({m}_{g}/{M}_{\odot }\right)}^{-1/6}﹩. Also shown is the sound speed for m1, which is essentially independent of resolution, and a power law of the form n−1/6 for reference. Bottom panel: same as the top panel, but for fc. The dashed lines show the solid curves scaled according to Equation (16).
Paper: Multilayered Fast Wind Observed in XMM-Newton Snapshot of Seyfert 1 Markarian 877
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, W. N. Brandt, Luigi Gallo, Doyee Byun, Elena Gallo
Figure caption: Top panel: the observed X-ray spectrum of Mrk 877 with the best-fit model (red curve), plotted relative to the underlying power-law continuum (orange curve) to highlight the absorption features. The contributions from each of the three “pion” components are shown separately by blue, magenta, and green curves, respectively. Bottom three panels: the transmission models of each “pion” component plotted individually, with vertical lines marking the most prominent absorption lines from different elements. The bottom panel for “pion#3” is plotted in a range of 0.3–3 keV, while all other panels are plotted in a range of 0.3–10 keV.