adsabs/AstroCLIMB huggingface dataset:
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Same as Figure 21 for the Bright Northern Ridge.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The N19 (black) and Bright Northern Ridge (white) masks contoured over the 160 μm image.
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: (a). Light curve of SMC X-1 obtained with NinjaSat (black dots), MAXI (green triangles), and Swift/BAT (orange squares). NinjaSat data collected during orbital eclipses are shown in green. The light gray shaded regions indicate the superorbital ascending (MJD 60657–60662) and descending (MJD 60688–60695) states, while the dark gray region marks the superorbital low state (MJD 60695–60704). 11 observed orbital cycles are labeled “i” to “xi.” (b). Hardness ratio (10–20 keV/2–10 keV) derived from NinjaSat observations. (c). Evolution of pulse arrival phases relative to a quadratic ephemeris with ﹩\dot{\nu }=2.668\times 1{0}^{-11}﹩ Hz s−1, based on the average spinup rate during this superorbital cycle. The red curves denote the best-fit quadratic (cycles i to ii) and fourth-order polynomials (cycles iv to ix). (d). Spin period deviations relative to the quadratic model. The spin periods for each orbital cycle are derived from TOA fitting (black points) and cross-validated using the ﹩{Z}_{2}^{2}﹩-test (orange diamonds). (e). Evolution of the local ﹩\dot{\nu }﹩. The red curves in panels (d) and (e) are derived from the timing solutions in panel (c).
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Long-term spin evolution of SMC X-1 observed with NinjaSat and MAXI. (a). The 2–20 keV MAXI 6 hr binned light curve is plotted in blue, and the scaled 1 day binned Swift/BAT light curve is plotted in orange. (b). Spin-frequency (ν) evolution. The blue triangles represent values averaged over individual superorbital high states using MAXI data; the gray squares show values computed over 8–12 days intervals; and the black dots indicate NinjaSat measurements for each binary orbital cycle. The black dashed line is a linear fit to the 8–12 days MAXI ν measurements. (c). Residuals of ν after subtracting the best-fit linear trend shown in panel (b). (d). Evolution of the spinup rate (﹩\dot{\nu }﹩). The dashed line represents the best-fit average ﹩\dot{\nu }﹩ across the nine superorbital cycles, as determined from the linear model in panel (b).
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Spectral evolution of SMC X-1 during the NinjaSat monitoring campaign from 2024 December to 2025 January. (a) The 2–20 keV light curve is presented as a reference. (b)–(e) The corresponding evolution of spectral parameters derived from the best-fit pcfabs∗cutoffpl model: (b) NH from the pcfabs component; (c) partial covering fraction; (d) photon index (Γ); and (e) unabsorbed flux (2–20 keV band).
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Pulse profile evolution of SMC X-1 observed with NinjaSat. Pulse profiles for 11 orbital cycles (i to xi) are shown sequentially and color-coded, with their corresponding superorbital phase ranges labeled. Photon events from orbital eclipses and preeclipse dips were excluded from the folded light curves. The right panel displays the NinjaSat light curve. The black dots indicate data during orbital eclipses, while out-of-eclipse points are color-coded according to orbital cycle. The dotted lines mark the boundaries of the out-of-eclipse intervals for each orbital cycle. Preeclipse dips in cycles ix and x are marked by the gray filled regions. The photons collected during these intervals were excluded from the pulse profiles.
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Flux dependence of the peak ratio (a), PF of P1 (b), and PF of P2 (c). The gray arrows indicate the evolutionary track of each parameter from orbital cycle i through ix. The right panels show probability density distributions from Monte Carlo simulations (blue) and bootstrapped samples (orange).
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Three example spectra observed with NinjaSat. The spectrum during the ascending state corresponds to the first data point in Figure 5; the high-state spectrum is taken from the seventh point; and the low-state spectrum is from the last data point. The bottom panel displays residuals normalized to data uncertainties. Spectra are rebinned for display, to maintain a signal-to-noise ratio above 5 for display purposes.
Paper: Unveiling the Nature of Superorbital Modulation of SMC X-1 Using NinjaSat
Authors: Chin-Ping Hu, Naoyuki Ota, Takuya Takahashi, Tomoshi Takeda, Teruaki Enoto, Toru Tamagawa, Biswajit Paul, Sota Watanabe, Wataru Iwakiri, Tatehiro Mihara, Amira Aoyama, Satoko Iwata, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Mayu Ichibakase
Figure caption: Correlation between ﹩\dot{\nu }﹩ and 2–20 keV flux. No statistically significant correlation was observed from either Monte Carlo simulations or bootstrap resampling.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: The ALMA CO(3–2) line integrated moment-0 map of J0846.BG consisting of 18 lensed detections at z  =  2.660–2.669 all within 60″ of each other. Their associated 1D spectra for each detection is displayed in Figure 2. Each detection is labeled based off their image system designation (see Section 4.1). In total, these 18 CO images originate from 11 unique sources. The red ellipse in the bottom right represents the synthesized beam.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: CO(3–2) moment-1 velocity maps for various sources in the J0846.BG. The left panel of each set displays the HST F160W image with a 3σ contour outline of the integrated CO(3–2) line moment-0 maps. In the right panel of each set, we show the moment-1 velocity map with the same moment-0 contour overlaid. The color bar on the right of each set represents the corresponding velocities in kilometers per second. In each stamp, we provide a scale bar equating to 1″ in the bottom left and the synthesized beam in the bottom right, with the same orientation as in Figure 3.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: The J0846 field. Main panel: the 18 CO(3–2) moment-0 detections (magenta contours) at z  =  2.660–2.669 (J0846.BG) plotted over the HST/F160W imaging. The red ellipse in the bottom right represents the synthesized beam. The CO emission that makes up the ID7.2 images are only detected in <3 channels, but we display them here, as they have crucial implications on the lens model (see ID7 description in Section 4.1). In the blue contour, we provide the critical curve at z  =  2.67 of the lens model. Right panels: insets across J0846 that have VLA 6 GHz continuum emission (green contours) and outline (black) of the moment-0 map. This includes two foreground cluster (J0846.FG) galaxies, one of which is hosting a radio wide-angle tail.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: The source plane reconstruction of J0846.BG, 11 CO(3–2) member galaxies at z  =  2.67 plotted over the corresponding caustic curve (in black) from the lens model. Their respective color indicates the velocity offset relative to the average velocity for all member galaxies. The measured FWHMs from each source’s CO profile are reflected in their relative sizes on the plot. In the bottom-right inset, we display the velocity histogram of all galaxies. We find that these 11 CO galaxies reside in a physical area of 150 kpc × 280 kpc all within a velocity offset of ΔV ≈ 800 km s−1, and velocity dispersion of σv  =  246 ± 72 km s−1. The center of the plane at x  =  0, y  =  0 corresponds to the WCS coordinate at R.A. = 131.70877, decl. = 15.09936.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: Color–magnitude diagram using r′ and z′, covering rest-frame 3500 and 5068 Å at z  =  0.77, respectively, effectively bracketing the 4000 Å break. All stars have also been removed on the plot via FWHM selection criteria. The red and green stars are spectroscopic objects at the cluster redshift and outside of it, respectively. The spec−z object circled in blue indicates the bright foreground elliptical at z  =  0.357. The red horizontal lines indicate our color cut selection to identify the cluster red sequence also imposing a magnitude cut at ﹩{m}_{z^{\prime} }\,=\,21.7﹩.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: ALMA 1D spectra for all 18 CO(3–2) line detections with their best-fit multi-Gaussian profiles plotted in the magenta curve (residual is plotted in the blue points). All detections are within the redshift range of z  =  2.660–2.669, equating to ΔV ≈ 800 km s−1 of each other. The central velocity, ΔV  =  0 km s−1, corresponds to z  =  2.666, the central redshift of this system.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: Left panel: the global modified blackbody dust SED model fit for J0846.BG, utilizing the unresolved dust continuum measurements (from K. C. Harrington et al. 2021; D. A. Berman et al. 2022). We plot the best-fit model (red curve) and 1000 randomly sampled models from the MCMC posterior (gray curves), as well as the photometric data points (blue points). Right panels: corner plot displaying the posterior likelihood distribution for the parameter space of the modified blackbody model fit. The dashed lines on the 1D posterior distribution represent the 16th, 50th, and 84th percentiles.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: Optical spectroscopic redshifts plotted over the F160W image. The cluster (J0846.FG) member galaxies within z  =  0.75–0.772 are shown with their corresponding color-scale (filled circles). The green stars indicate objects that have redshift measurements outside the cluster redshift, all at z < 0.4.  The bright elliptical circled in blue indicates a foreground perturber at z  =  0.357.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: The identified non-CO-emitting image systems (ID12, ID13, and ID14). Left panel: color image using r′, z′, F160W. Right panel: F160W image with the foreground galaxy (green “×” symbol) subtracted utilizing GALFIT. Labeled are the four images of the Einstein Cross, illustrating the flip in parity with the comma-like morphology. For reference, the FOV corresponds to the bottom panel of Figure 4, in the vicinity of image systems 4 and 6.
Paper: PASSAGES: The Discovery of a Strongly Lensed Protocluster Core Candidate at Cosmic Noon
Authors: Nicholas Foo, Kevin C. Harrington, Brenda L. Frye, Patrick S. Kamieneski, Min S. Yun, Massimo Pascale, Ilsang Yoon, Allison Noble, Rogier A. Windhorst, Seth H. Cohen, James D. Lowenthal, Melanie Kaasinen, Belén Alcalde Pampliega, Daizhong Liu, Olivia Cooper, Carlos Garcia Diaz, Anastasio Díaz-Sánchez, Jose Diego, Nikhil Garuda, Eric F. Jiménez-Andrade, Reagen Leimbach, Amit Vishwas, Q. Daniel Wang, Dazhi Zhou, Adi Zitrin
Figure caption: For comparison with J0846.BG (plotted with a star), the total SFRs (y-axis) are shown for different protocluster cores with known DSFGs at varying redshifts (x-axis) reported in S. Alberts & A. Noble (2022). The color bar denotes the number of DSFGs that are identified for each system.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Flux and polarization spectra for our SN 2012au observations. The relative flux spectra are in black, and polarization spectra (binned to 15 Å) are in purple with error bars shaded. Polarization spectra are not ISP or continuum subtracted; we note that from reddening considerations the maximum possible ISP is 0.66% (see Section 4). The rest wavelengths of prominent features in the spectra are marked by vertical lines and color coded according to atomic species. The gray-shaded regions span the ranges where we measured the continuum polarization for each epoch (Section 5).
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: ISP estimates (Section 4) displayed on the q−u plane for comparison. The ISP magnitude calculated from the Serkowski-reddening maximum relationship is shown as a red circle to indicate no specific PA. The pink cross is the value of probe star HD 112142. The purple cross represents the value of the most distant probe star HD 112325. The small green cross represents the estimate presented in S. Pandey et al. (2021). The yellow cross is the estimate we obtain from our days 85−90 continuum region (Section 5). The sizes of these crosses denote the uncertainty of each estimate. The solid blue and gray lines are the best-fit lines to our data from days 0−7 and 295, respectively, with the 5σ errors shown as shaded regions around them.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: SN 2012au flux spectra over days 0–295 post-R-band max, collected by the SNSPOL project. Flux spectra have been adjusted after flux calibration to stack neatly and used to identify key line features (labeled).
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 center panel shows the u–v midpoint of all runs and telescope pairs, with different-color shaded regions indicating angular slices in the u–v plane. For data within each of the individual slices, the surrounding panels of corresponding colors show the squared visibility as a function of the length of the baseline. Each slice is fit with a uniform disk model to extract the effective one-dimensional radius of a given angular projection. The zero-baseline squared visibility is constrained to be the same for all slices, with a value from the uniform ellipse fit of Figure 9. Identical lightly shaded regions in each panel show the range of fits between the most extreme values of the eight individual slices; these are drawn to guide the eye, making small differences between panels more apparent. A data point at a large baseline in slice 5 is drawn in red and discussed in the text.
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 area of the fitted correlation peak, proportional to the squared visibility, as a function of the magnitude of the baseline. The curve represents the best fit with a uniform disk model. Points in gray, excluded from the fit, are below the threshold where the signal/noise is too low to reliably detect peaks, as discussed in Section 3.6. This threshold is marked with a gray shaded box.