adsabs/AstroCLIMB huggingface dataset:
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: Color–color plots of ASASSN-21qj using the log-normal size distribution to calculate reddening vectors for a dust cloud occulting the star. Six materials out of the twelve materials tested are presented in this figure. The top two rows show the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -i^{\prime} ﹩ plots, while the bottom two rows show the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -z^{\prime} ﹩ plots. The LCOGT colors are presented as blue or orange data points, with the unreddened color expected of a G2 V star shown as the yellow “⋆” symbol. Blue or orange dashed lines denote the reddening vectors for distributions of grains with different peak sizes between 0.1 and 1.2 μm consistent with the observations. The solid line denotes the vector for the best-fitting size for each material taking into account both the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -i^{\prime} ﹩ and ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -z^{\prime} ﹩ colors.
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: Color–color plots of ASASSN-21qj using the power-law size distribution to calculate reddening vectors for a dust cloud occulting the star. Six materials out of the twelve materials tested are presented in this figure. The top two rows show the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -i^{\prime} ﹩ plots, while the bottom two rows show the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -z^{\prime} ﹩ plots. The LCOGT colors are presented as blue or orange data points, with the unreddened color expected of a G2 V star shown as the yellow star symbol. Blue or orange dashed lines denote the reddening vectors for distributions of grains with different minimum sizes between 0.1 and 1.2 μm consistent with the observations. The solid line denotes the vector for the best-fitting size for each material taking into account both the ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -i^{\prime} ﹩ and ﹩g^{\prime} -r^{\prime} ﹩ vs. ﹩r^{\prime} -z^{\prime} ﹩ colors.
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: Close-up of the ASASSN-21qj occultation events presented in Figure 1 from MJD 59,450 to 59,750. Here we present multiwavelength measurements comprising ﹩g^{\prime} ﹩ (green), ﹩r^{\prime} ﹩ (red), ﹩i^{\prime} ﹩ (blue), and z (orange). The unocculted magnitude of the star in each filter is denoted by the dashed line in the respective color. Vertical dashed gray lines denote the postulated period of 30.9 days based on the first two deep events and their predicted recurrence.
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: Color–color plots of ASASSN-21qj highlighting the fitting results for amorphous pyroxene (Mg1.6Fe0.4Si2O6); on the left is ﹩g^{\prime} ﹩-﹩r^{\prime} ﹩ vs. ﹩r^{\prime} ﹩-﹩i^{\prime} ﹩, and on the right is ﹩g^{\prime} ﹩-﹩r^{\prime} ﹩ vs. ﹩r^{\prime} ﹩-﹩z^{\prime} ﹩. In each panel the LCOGT photometry (colors) are denoted by circular data points, while the star symbol denotes the photospheric colors for a Sun-like star. We omit data points of the deepest occultations from this graph, focusing here on fitting the reddening due to the bulk of the dust. Reddening lines for power-law (solid) and log-normal (dashed) size distributions that fit the observations are shown as colored lines. The best-fit lines for each distribution are shown as black lines.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Thermal equilibrium solutions at R = 5R s (left), R = 10R s (middle), and R = 250R s (right) with λ = 0.5 and η = 2 on the mass accretion rate vs. surface density plane, in comparison with solutions from the Wu et al. (2022) model that does not consider the magnetic pressure. The four branches of solutions are marked.
Paper: Absorption Line Oscillator Strengths for the C 2Π(0)-A 2Σ+(0) Band of Nitric Oxide
Authors: A. M. Velasco, C. Lavín
Figure caption: Diabatic potential energy curves for the C 2Π, B 2Π and A 2Σ+ states of NO.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of source term associated with the evolution of PUI energy along the x-axis from 70 to 140 au in Models 1 (red dots) and 2 (blue plus symbols).
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Power-law radial dependence p of the mass accretion rate as a function of radius for four solutions found at different mass accretion rates. At ﹩{\dot{m}}_{10}=0.01﹩, the inner disk is in the ADAF branch while the outer disk is in the SSD branch. A self-consistent constant p can be obtained in a wide range of radii except for the near-critical case with ﹩{\dot{m}}_{10}=1﹩.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Disk scale height (H/R), surface density (Σ), total optical depth (τ), ion temperature (T i), radial velocity (−V  R ), and angular velocity (Ω/ΩK) as a function of radius in the slim disk (﹩{\dot{m}}_{10}=100﹩), SSD (﹩{\dot{m}}_{10}=0.01﹩), and ADAF (﹩{\dot{m}}_{10}=0.01﹩) solutions.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Fractional cooling through advective (f adv), radiation (f rad), and outflow (f w) as a function of radius, in the slim disk (﹩{\dot{m}}_{10}=100﹩), SSD (﹩{\dot{m}}_{10}=0.01﹩), and ADAF (﹩{\dot{m}}_{10}=0.01﹩) solutions.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Radial profiles of the gas, radiation, and magnetic pressures in the slim disk (﹩{\dot{m}}_{10}=100﹩), SSD (﹩{\dot{m}}_{10}=0.01﹩), and ADAF (﹩{\dot{m}}_{10}=0.01﹩) solutions.
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: JCMT-SCUBA-2 850 μm images of the surrounding regions around 54 z ∼ 6 quasars with a beam size of FWHM = 15″. The selected region is within 2.′23 from the quasar optical position (which covers typical protocluster scales at z ∼ 6) and has 1σ uncertainty of <1.5 mJy beam−1 for each pixel. The contour levels are +3, +4, +5, +6, +7 × 1.5 mJy beam−1 for each map. The stars indicate the quasar optical/NIR position. The stars with the blue edge are the submillimeter-detected quasars. The blue circles indicate the selected SMGs (with S/N > 3.5 at 850 μm or 450 μm; see Table 2). The sources marked with “#” are the SMGs used in the overdensity analysis with deboosted fluxes >5.5 mJy. The JCMT-SCUBA-2 850 μm FITS images shown in this figure are available as the Data behind the Figure. The 450 μm FITS images are also included.
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: Example completeness and flux boosting estimates based on Monte Carlo source insertion. Left: completeness as a function of input flux (S in). The solid curve represents the best-fit function of f(S in) = [1 + erf((S in – A)/B)]/2, with best-fitting parameters given in the text. Right: the ratio between input flux density and output flux density as a function of input flux. Error bars show 1σ of 5000 trials. The solid curve represents the best-fit function of f(S in) = 1 + A exp(–BS                         ﹩{}_{\mathrm{in}}^{C}﹩) (Hatsukade et al. 2016).
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: Example SCUBA-2 exposure time map. The contours denote the 20%, 40%, and 60% exposure time levels compared to the maximum level on the map. The blue circle region has a diameter of 4′ and marks the region with uniform and low rms for SMG overdensity searches.
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: The S/N histograms of the signal maps in the field of quasar SDSS J0100+2802 (z = 6.3258 ± 0.0010) in the 850 and 450 μm bands. The dashed and solid lines indicate 3.5σ and 4σ, respectively. The red line represents the Gaussian fitting of the noise statistics.
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: The distribution of the map depth at 850 and 450  μm.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Rest-frame weighted biweight-averaged stack of ∼50,000 LAEs from HPSC-1 between 1.9 < z < 3.5 (not corrected for IGM transmission). The spectrum has been smoothed with a 1 pixel (0.44 Å) Gaussian kernel (σ). As noted in Section 3.4, the number of contributing galaxies (Figure 3 green curve, bottom panel) decreases with distance from Lyα, dropping to 16% in the extreme blue and 4% in the red. The uncertainties (Figure 3 orange curve, top panel) are ∼5% except for near edges of the wavelength range where they rise to ∼25% at the red end and ∼100% in the far blue. Despite containing more contributing spectra, the blue end of the spectrum has larger uncertainties due to the performance of the CCD (Gebhardt et al. 2021). These uncertainties are defined as ﹩{\sigma }_{b}/\sqrt{{n}_{\lambda }}﹩ where σ  b  is the biweight scale and n  λ  is the number of spectra contributing to the wavelength bin. The inset in the upper right shows the full height of the Lyα line in the same luminosity units. The deep troughs near the Lyα line have some physical motivation, but are artificially enhanced by the data-reduction pipeline (see Section 4.4). This spectrum, with the associated error array, is available in electronic form.(The data used to create this figure are available.)
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Weighted biweight average of the residuals produced by sky subtraction derived from stacking more than 300,000 random, empty 3.″5 radius apertures taken from HPSC-1 HETDEX observations. The errors are shown in gray and are derived via ﹩{\sigma }_{b}/\sqrt{N}﹩ where σ  b  is the biweight scale. The f  λ  level of this residual spectrum is ∼1% of the HETDEX flux limits (Gebhardt et al. 2021), and thus, meaningful only when stacking large numbers of spectra. The rise in the far blue end of the spectrum is primarily due to a limitation in the instrument and the slightly negative flux redward of ∼4000 Å is a result of a small overcorrection in the sky subtraction. The spectrum is available in electronic form.(The data used to create this figure are available.)
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Rest-frame weighted biweight-averaged stack of ∼50,000 LAEs from HPSC-1 between 1.9 < z < 3.5 (not corrected for IGM transmission), as in Figure 2, with the uncertainty shown in orange (top panel) and the number of contributing galaxies per wavelength bin in green (bottom panel).
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption:                    ﹩\tfrac{1/{{\rm{\Gamma }}}^{2}}{{\rm{\Delta }}r/r}﹩ at the final frame of the 16TI HD simulation. Quantities > > 1 mean that detected photons are sufficiently able to probe the smallest spatial scales of the jet.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Light crossing over HD cell size ratio at the beginning of the simulation. Panel (a) shows ﹩\tfrac{c/{fps}}{{\rm{\Delta }}r}=\tfrac{c{\rm{\Delta }}t}{{\rm{\Delta }}r}﹩ at the first moment of photon injection (﹩{t}_{\mathrm{sim}}=50﹩ s). Panel (b) shows ﹩\tfrac{c/{fps}}{{\rm{\Delta }}r}=\tfrac{c{\rm{\Delta }}t}{{\rm{\Delta }}r}﹩ at the end of the simulation (﹩{t}_{\mathrm{sim}}=527.6﹩ s).
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, 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, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Spectral distribution plot with the best-fit leptonic (blue) and hadronic (red) scenarios for SNR G28.6−0.1.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: Comparison of the BS radius at the terminator found from studies using VEX (orange dots; this study), PVO (blue squares; Russell et al. 1988), and Venera 9/10 (green diamond; Smirnov et al. 1980). The gray line shows the monthly average SSNs, a proxy for the solar cycle.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: Distances to the system of pulsar J1732–5049 and its candidate binary companion. These Gaia parallaxes are the first potential measurements to the pulsar. Both parallax distances are more than double either DM distance (based on NE2001 in blue or YMW16 in yellow), which assume a standard error of ±20%. This may indicate that these models have overestimated the electron density along this line of sight.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: Panels (a) through (d) show comparisons of the location of J1747–4036 (red) and candidate companion objects (blue) after updating the Gaia object positions to the IPTA epoch. Both objects’ positions are consistent with the IPTA position of J1747–4036. Panel (e) shows distances to the system of J1747–4036 in DR3. DM distances from NE2001 (blue strip) and YMW16 (yellow strip) are shown for illustrative purposes and are not included in the combined measurements.
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: A color–magnitude plot displaying six of the companions to pulsars from this cross-match (orange) against a background of well-measured stars in the Gaia catalog.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Model spectra at 0.5, 1.0, and 2.0 days for the model TSvw0.5vd2 from Korobkin et al. (2021) along two different viewing angles (along the angular momentum axis and perpendicular to this axis).
Paper: Improving Distances to Binary Millisecond Pulsars with Gaia
Authors: Abigail Moran, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, David N. Spergel
Figure caption: False association: the sky position of J1949+3106 (red IPTA bar) as compared to the object identified in Gaia DR2 as the pulsar’s companion (pink). The Gaia DR3 data (blue) illustrate that this was a false association. The Gaia object’s position differs from the pulsar’s by 22σ in R.A. and 2.2σ in decl. (a) R.A. of J1949+3106’s former Gaia match, (b) decl. of J1949+3106’s former Gaia match.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Trial LIGO alert as processed by DIAGNOSIS for local distribution.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Phase II TSL generated by DIAGNOSIS giving the prioritized list of target galaxies that will be employed to trigger the search for the OT with the VIRUS IFU array. The galaxies in this list are also presented in Figure B3.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: SMHM relation for quenched galaxies at different redshifts: z = 0, top left; z = 1, top right; z = 2, bottom left; and z = 3, bottom right. Violet points, galaxies from the catalog; red line, SMHM relation from abundance matching at z = 0; blue line, relation M ⋆ = 0.16 M H. Top panel: quenched galaxies selected randomly. Bottom panel: quenched galaxies selected by their distance from M ⋆ = 0.16 M H relation. We can notice that, at given redshift and stellar mass bin, a random selection of galaxies to activate between z and z + dz can give origin to some galaxies with above the blue line. We can avoid this issue by selecting galaxies to activate between the nearest to the M ⋆ = 0.16 M H relation.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Example of evolution of bulge and disk for two galaxies. Black line, halo mass; red line, total stellar mass; orange line, bulge mass; blue line, disk mass. Dashed vertical line represents the moment of transition between fast and slow accretion z FS. Top panel shows a quenched galaxy with z  Q  > z FS; all the stellar mass in the bulge and the galaxy is an elliptical. Bottom panel shows a star-forming galaxy building its bulge up to z FS ≃ 1.5 and the disk at lower redshift.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: SMF for quenched galaxies. Colors are as in Figure 1. Histograms are the SMF for surviving haloes, dashed lines the total SMF reconstructed from our catalog, and solid lines the fit by Davidzon et al. (2017). By construction, our model tracks the evolution of the quenched galaxies SMF.