adsabs/AstroCLIMB huggingface dataset:
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: M87 light curves for different timescales. The black points represent the calculated fluxes with a significance of ≥2σ, while the gray points represent the calculated fluxes with a significance of <2σ. Top: daily light curve (LC). Middle: weekly LC. Bottom: monthly LC.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Evolution of the sample galaxies in the UVJ diagram across different redshift bins (0 < z < 4). Each row represents different radial regions: inner (r < 4 kpc; top row) and outer (r > 4 kpc; bottom row). Each panel shows the density of galaxies in U − V and V − J color space for the corresponding radial region, visualized using filled contours. The orange star in each panel indicates the median value. The dashed, dashed–dotted, and dotted black lines indicate the quiescent region from R. J. Williams et al. (2009), the separator line of fully quenched and recently quenched galaxies from O. Almaini et al. (2017), and the extended region for recently quenched galaxies from Z. Mao et al. (2022), respectively. The evolutionary tracks for slow (blue dashed) and fast (red dashed–dotted) quenching models are overlaid for comparison. Red and blue crosses mark the positions of galaxies at ages of 1, 2, 3, 4, and 5 Gyr. Median U − V and V − J color errors, shown in the lower right corner of each panel, are estimated from observed fluxes using filters with rest-frame wavelengths closest to the U, V, and J bands. The black arrow in the top left panel indicates the dust attenuation vector corresponding to AV ∼ 0.5.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Radial profiles of stellar mass surface density (Σ*; top row), SFR surface density (ΣSFR; second row), specific SFR (sSFR; third row), U − V (fourth row), and V − J colors (fifth row) from piXedfit, color-coded by redshift. Thick lines represent the median values, while shaded regions indicate the 16th–84th percentile range. The fifth column presents the median profiles for each redshift bin. The dotted lines in the fifth column indicate the half-mass radius (top row). The solid red lines in the uppermost row show the largest PSF profile, obtained from F444W band.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Evolution of stellar mass in massive quiescent galaxies. The figure displays the median stellar mass for the inner (red), outer (blue), and total (black) regions across different redshift bins. Error bars indicate the scatter in the data, estimated through bootstrapping.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Color-composite images of the most massive galaxies in each redshift bin (see Section 4.3). These images are constructed using the estimated rest-frame U, V, and J bands fluxes derived from piXedfit, mapped to the blue, green, and red components, respectively. The method for estimating the rest-frame fluxes for each pixel is described in Section 4.2. Each panel is scaled to a physical size of ∼40 kpc. The redshift and estimated total stellar mass of each galaxy are indicated in the corresponding panel; spectroscopic redshifts are shown in green. Galaxies hosting X-ray-detected sources are labeled in orange.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Examples of RGB images (F150W+F200W+F444W; panels (a) and (e)), pixel-binning maps (panels (b) and (f)), stellar mass surface density maps (panels (c) and (g)), SFR surface density maps (panels (d) and (h)), and fitted SEDs in several bins of primer-cosmos-east-grizli-v7.0 #45144 (top right) and primer-uds-south-grizli-v7.2 #16789 (bottom right) derived with piXedfit. In the fitted SEDs, open squares represent the observed fluxes, while filled circles indicate the fluxes predicted by the best-fit model.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: The relationship between core stellar mass surface density (Σ*,1kpc) and total stellar mass for our sample. Colored and gray points represent our progenitor/descendant sample (Section 4.3) and the full sample, respectively. The blue, black, and red lines indicate fitted relations for the progenitor/descendant sample, the full sample, and empirical relations from previous studies, respectively (J. J. Fang et al. 2013; S. Tacchella et al. 2015).
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Predicted (solid black line) and observed stellar mass of our sample in Section 4.3. Red points represent galaxies selected using the extended UVJ selection, while blue points represent those selected using the original UVJ criteria. The predicted stellar mass evolutions are calculated with the abundance matching method using the nd-redshift code (P. S. Behroozi et al. 2013) and the stellar mass functions from I. K. Baldry et al. (2012), D. J. McLeod et al. (2021), and A. Weibel et al. (2024).
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Comparison of required specific mass growth rates (orange) with median of estimated sSFR (blue) for inner (leftmost column), outer (middle column), and total regions (rightmost column). Error bars indicate the scatter in the data, estimated through bootstrapping.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Number of bins per galaxy as a function of redshift. Blue points indicate the median values within each redshift bin.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Sketches of different dust configurations (shaded gray). Panel (a) shows a model for centrally concentrated extinction from C. Carr et al. (2021), and panel (b) shows one in which extinction originates exclusively from the central dense zone, which is much smaller than the radial extent of the emitting wind. In these two panels, the shown sight line s includes photons emitted from slower gas at smaller radius (orange) and fast gas at large radius (red); these originate from excitation by UV radiation from the SSC emitted over a larger range of θ for slow gas relative to fast gas. Panel (c) shows a model for dust distributed uniformly within the wind volume. For the shown sight line (straight arrow), the blueshifted path length is given by s1 and the redshifted one by s1 + 2s2. For the model in panel (d), the extinction originates from a slab across the center of the system. See the text for details on how these models affect the emission-line profiles.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: LyC photons escape through gaps in the dense, fragmented shell (green) surrounding the parent cluster and drive a superwind composed of tiny neutral gas clumps with a low filling factor. These radiation-driven wind clumps continue to absorb photons and accelerate, reaching higher speeds at larger radial distances (arrows), corresponding to, respectively, larger Doppler shifts (red and blue color-coding). The dense clouds have a slow, momentum-conserving outward motion driven by the weak stellar winds.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Power-law slopes αblue and αred, and the slope difference Δα vs. absorbed LyC luminosity (top panels), B − V color excess (middle panels), and oxygen abundance (bottom panels). The points are color-coded by ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Oxygen abundance vs. ﹩\mathrm{log}({{\rm{O}}}_{32})﹩ of the galaxies in our sample, color-coded by ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩, with different symbols representing the wing morphologies.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Power-law slopes αblue and αred of the broad emission-line wings vs. observed LyC luminosity (top panels), LyC escape fraction (middle panels), and Lyα escape fraction (bottom panels). The points are color-coded by ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩ and sized by E(B − V).
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Oxygen abundance vs. EW(Hβ), color-coded by ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩, with different symbols representing the wing morphologies.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Left panel: observed LyC luminosity vs. normalized broad-wing luminosity L≥300/Ltot. Right panel: LyC escape fraction ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩ vs. L≥300/Ltot.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Blue- and red-wing power-law slopes αblue and αred vs. EW(Hβ) (top panels), EW(Lyα) (middle panels), and O32 (bottom panels). The points are color-coded by the absorbed LyC luminosity.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Normalized broad-wing luminosity vs. light fraction of <3 Myr old stellar populations, color-coded by ﹩{V}_{{\rm{Max}}}﹩.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: Observed redshift (upper left), luminosity (upper right), photon index (lower left), and intrinsic cumulative source-count (lower right) distributions of LAT FSRQs. The solid line is the best-fit line of the LDDE model, including the effects of selection bias, to compare with the observed data. The error bars represent the statistical uncertainties based on Poisson statistics. In the case of zero sources in a given bin, the 1σ upper limits are shown (see N. Gehrels 1986). The red data points (lower right), showing the intrinsic source-count distribution, are calculated using the sky coverage. The corresponding error bars show the propagated errors, including the statistical uncertainty and the uncertainty in the sky coverage.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The evolution of the Fermi FSRQs subdivided into six bins in luminosity, constructed using the Nobs/Nmdl method, by employing the best-fit (LDDE) model. The peak in evolution is at a higher redshift for a more luminous class—that is, this plot shows the luminosity dependence of the evolution in density. The systematic uncertainty shown in the blue shaded region is derived using the detection efficiency (see Section 3.5).
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: Observed redshift (upper left), luminosity (upper right), photon index (lower left), and intrinsic cumulative source-count (lower right) distributions of LAT FSRQs. The solid line is the best-fit line of the PLE model, including the effects of selection bias, to compare with the observed data. The error bars represent the statistical uncertainties based on Poisson statistics. In the case of zero sources in a given bin, the 1σ upper limits are shown (see N. Gehrels 1986). The red data points (lower right), showing the intrinsic source-count distribution, are calculated using the sky coverage. The corresponding error bars show the propagated errors, including the statistical uncertainty and the uncertainty in the sky coverage.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The LF of the Fermi FSRQs subdivided into four bins in redshift, constructed using the Nobs/Nmdl method. The solid lines depict the best-fit model (LDDE) in each redshift bin, along with the space density in the previous bin, given by the dashed line for comparison. The systematic uncertainty shown in the blue shaded region is derived using the detection efficiency (see Section 3.5).
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: Observed redshift (upper left), luminosity (upper right), photon index (lower left), and intrinsic cumulative source-count (lower right) distributions of LAT FSRQs. The solid line is the best-fit line of the PDE model, including the effects of selection bias, to compare with the observed data. The error bars represent the statistical uncertainties based on Poisson statistics. In the case of zero sources in a given bin, the 1σ upper limits are shown (see N. Gehrels 1986). The red data points (lower right), showing the intrinsic source-count distribution, are calculated using the sky coverage. The corresponding error bars show the propagated errors, including the statistical uncertainty and the uncertainty in the sky coverage.
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: Scaled radial displacement eigenfunctions corresponding to the observed frequencies in the best-fitting model. Panel (a) corresponds to the fundamental radial mode F22; panel (b) to the first radial overtone mode F1; panels (c), (d), (e), (f), and (g) correspond to the observed frequencies F6, F3, F2, F7, and F13, respectively. The vertical red dashed lines mark the boundary of the convective core (∇r = ∇ad).
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: Visualization of the Brunt–Väisälä frequency (N), characteristic acoustic oscillation frequencies (Sℓ for ℓ = 2, 3), and hydrogen abundance (XH) inside component B. The vertical dashed line indicates the boundary of the convective zone (∇r = ∇ad).
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The intrinsic differential source-count distribution (logN–logS) of FSRQs plotted against the energy flux. The solid blue line represents the intrinsic logN–logS as derived using the LDDE model. The data points are calculated using Equation (21). The error bars show the propagated errors, including the statistical uncertainty and the uncertainty in the sky coverage.