adsabs/AstroCLIMB huggingface dataset:
Paper: Gnuastro: Estimating the Zero-point Magnitude in Astronomical Imaging
Authors: Sepideh Eskandarlou, Mohammad Akhlaghi, Raúl Infante-Sainz, Elham Saremi, Samane Raji, Zahra Sharbaf, Giulia Golini, Zohreh Ghaffari, Johan H. Knapen
Figure caption: Difference in magnitude (using apertures of radius 2″ and 6″) as a function of the reference magnitude for stars in the input image. The horizontal range of this plot shows the zero-point magnitude and its scatter. In both cases SDSS DR12 is used as a reference: the left panel uses an SDSS image and right uses on the SDSS catalog overlapping with our input image. In right panel (from a catalog), stars brighter than the 15th magnitude are present because the SDSS pipeline attempts to find the magnitude of saturated stars (which is not done in the left panel). The blue and yellow filled circles have a smaller dispersion (σ in legend). The zero-point magnitudes are obtained based on the horizontal component of the blue and yellow filled circles with lower σ (within the magnitude range that is shown with the red vertical lines). The underlying data for creating the left and right panels are available in Zenodo doi:10.5281/zenodo.10256845 (files with the .txt suffix).
Paper: Concerning the Verity of the MMRD Relation for Novae
Authors: Allen W. Shafter, J. Grace Clark, Kamil Hornoch
Figure caption: The MMRD plane divided into four quadrants: Q1–Q4. The filled black circles show data for Galactic novae from Downes & Duerbeck (2000). The dashed line is the best linear fit to these data. The blue squares show Galactic RNe from Schaefer (2010), while the red diamonds show our updated M31 RN sample. Most classical novae discovered in routine nova patrols fall either in Q1 or Q4. Known RNe on the other hand fall almost exclusively in Q2, while Q3 is almost devoid of novae.(The data used to create this figure are available.)
Paper: New Abundance Determinations for the B9 Mn Star HD 53929
Authors: Richard Monier
Figure caption: Left: the Fe II lines of HD 53929 in the range 2560–2610 Å, Right: the Si II resonance doublet of HD 53929 at 1526.71 and 1533.43 Å.
Paper: CO Fundamental and First Overtone Emission in the Nova V496 Scuti
Authors: Richard J. Rudy, Ray W. Russell, Michael L. Sitko, Lawrence S. Bernstein, William L. Dimpfl, Karen S. Bjorkman, John P. Wisniewski
Figure caption: Observations and modeling of the carbon monoxide (CO) emission of the nova V496 Scuti from 15.5 days after maximum light. The top panel shows the observations of the CO fundamental and first overtone from 2009 December 4. Most of the atomic emission lines are H I lines from the Brackett and Pfund series with some features from C I detectable as well. The spectral regions shortward of 2.29 μm and between 3.4 and 4.0 μm establish the continuum level and demonstrate the excess emission due to the carbon monoxide fundamental and first overtone. The middle panel displays an enlargement of the CO first overtone observations and model. The modeled CO emission is plotted with a vertical offset to facilitate comparison with the measured spectrum. Grid lines show the location of the CO bandheads for both 12CO and 13CO. An unidentified feature at 2.37 μm is marked. The model is for a 13C/12C value of 0.7 and a gas temperature of 4000 K. The bottom panel shows the modeled CO fundamental and first overtone (with no offset) together with the observations. Also shown is an optically thin model, normalized to first overtone, that illustrates the profound change to the shape and intensity of the fundamental that results from the optical depth.(The data used to create this figure are available.)
Paper: The CO(6−5) Protostellar Jet Driven by HH 212 as Imaged by ALMA-Band 9
Authors: C. Codella, F. Gueth, S. Cabrit
Figure caption: The HH 212 jet. Left: dust continuum emission (black) overlaped with the CO(6–5) line emission at ±2 km s−1 with respect to V sys, plot in magenta (LV). For continuum, first contour and steps are 5σ (51 mJy beam−1). For CO(6−5), first contour and steps are 3σ (0.90 Jy beam−1 km s−1) and 1σ, respectively. Middle: distribution of the red- and blueshifted CO(6−5) emission at velocities (with respect to V sys) larger than ±2 km s−1 (HV), down to –11 km s−1 (blue) and up to +12 km km s−1 (red). First contour and steps are 3σ (1.17 Jy beam−1 km s−1, blue, and 1.44 Jy beam−1 km s−1, red) and 1σ, respectively. Right: spectra of CO(6−5) extracted at the peak positions of the HV distribution (in both flux density, F  ν , and temperature brightness, T B). The vertical line indicates the systemic velocity.
Paper: Distance to Leo A Based on a Post-asymptotic-giant-branch Star
Authors: Chow-Choong Ngeow
Figure caption: The locations of star 03 (filled triangles) in the color–magnitude diagrams as compared to the four calibrating yellow PAGB stars used in (Ngeow et al. 2022, blue squares), when the distance modulus of star 03 was assumed to be 24.48 mag (as measured from RR Lyrae in Bernard et al. (2013), the red triangles) and 24.77 mag (as measured from blue supergiants in Urbaneja et al. (2023), the orange triangles), respectively. The horizontal lines represent the constant gr-band absolute magnitudes, and the dashed lines are for the case of linear gr-band absolute magnitudes, both were calibrated in Ngeow et al. (2022).
Paper: Clarifying the Optical Thin-lens Equations of Gravitational Self-lensing
Authors: Dimitris M. Christodoulou, Silas G. T. Laycock
Figure caption: Schematic diagram of a SL binary at its closest angular approach ﹩{\theta }_{\min }﹩. Observer O and lens L specify the LoS as the optical axis onto which we project the source at S. Angle ψ, the inclination of the binary orbit to the LoS, is exaggerated; also note that D OL ≫ D LS. The asterisk denoted by CM is the center of mass, a is the separation, and ﹩{\boldsymbol{ \mathcal L }}﹩ is the angular momentum vector of the binary. Image distance D LI (Equation (3)) is also exaggerated.
Paper: Hidden Companions to Intermediate-mass Stars. VIII. Discovery of a 0.6 M ⊙, 1.7 au Companion to Albali = ϵ Aquarii 
Authors: Idel Waisberg, Ygal Klein, Boaz Katz
Figure caption: Interferometric data (colored) and best fit binary model (black) for Albali = ϵ Aqr. The dashed lines show the expected values for a single star.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Dwarf galaxy detection sensitivity for each detection method individually (left and middle) and both methods combined (right). Detection rates have been corrected according to visual inspection results, where only artificial dwarfs that were classified as dwarfs by at least two people were counted as detections. Each bin contains, on average, 30 injected dwarfs with a standard deviation of 4. The corresponding average uncertainty in detection rate (calculated using binomial statistics) is 0.05. Lines of constant surface brightness are shown in gray (given in mag arcsec−2). When convolved with the dwarf galaxy size–luminosity relation (C. M. Brasseur et al. 2011), we are ∼80% complete for MV ≲ −7.8 and ∼50% complete for MV ≲ −7.0.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: 10σ PSF depth of DECam photometry around NGC 55 in g and i optical bands. 10σ PSF depth is defined as the PSF magnitude at which the signal-to-noise ratio is equal to 10. The central red regions correspond to fields with both DELVE-DEEP and DES imaging, while the outer blue regions correspond to fields with only DES imaging. The field in the bottom left corner was imaged as part of the DES supernova program and was excluded from our data set. The total region shown spans a projected physical radius of ∼150 kpc.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Binned color–magnitude diagram of the central region of NGC 55 with the RGB selection box used in our dwarf galaxy search displayed in red. This RGB box covers i-band magnitudes of 22.8 ≤ i ≤ 25.0. An isochrone corresponding to stellar populations with age = 10 Gyr and metallicity [Fe/H] = −2 at the distance of NGC 55 is shown in magenta, which was generated using the Dartmouth Stellar Evolution Database (A. Dotter et al. 2008). Magnitude uncertainties (which come from the SourceExtractor parameter, MAG_ERR) are given in gray on the left.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: RGB density map of DELVE-DEEP’s NGC 55 footprint (rad = 3.25 deg) with binsize = 1.5 arcmin2. The color bar indicates the number of sources per bin. The two previously known NGC 55 satellites, NGC 55-dw1 and ESO 294–010, plotted in red and cyan, respectively. We note that, while ESO 294–010 is located slightly outside the DELVE-DEEP footprint, it lies just at the edge of the virial radius of NGC 55.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Four injected artificial dwarf galaxies of varying absolute magnitude, half-light radius, and effective surface brightness shown in i band. Green circles indicate sources detected by SourceExtractor. Left column: Artificial dwarfs detected by our semiresolved method. Right column: Artificial dwarfs detected by our resolved method.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Satellite LF for NGC 55 down to MV = −7 (∼50% completeness limit of our dwarf search) given by the gray-dashed line. ESO 294-010 is shown with a red star and NGC 55-dw1 is shown with a red circle. While NGC 55-dw1 is a confirmed satellite of NGC 55, it is not included as part of our LF due to it being outside the size range of our sensitivity. The orange and blue-shaded regions correspond to predicted satellite populations for an LMC-mass host, adapted from the 80% scatter in I. M. E. Santos-Santos et al. (2022) and 1σ scatter in G. A. Dooley et al. (2017), respectively. Both of these regions have been convolved with our observed sensitivity.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Absolute magnitude vs. half-light radius for known dwarf satellites. Open gray symbols indicate MW and M31 satellites from the compilation of A. B. Pace (2024). Open blue symbols indicate satellites of the LMC (E. Patel et al. 2020) or LMC analogs: M33 (S. C. Chapman et al. 2013; D. Martínez-Delgado et al. 2021; M. L. M. Collins et al. 2024; I. Ogami et al. 2024), NGC 2403 (J. L. Carlin et al. 2024), NGC 300 (D. J. Sand et al. 2024), and NGC 4449 (D. Martínez-Delgado et al. 2012; R. M. Rich et al. 2012). Open green symbols indicate satellites of SMC analogs: NGC 3109 (M. E. Sharina et al. 2008; D. J. Sand et al. 2015; A. Doliva-Dolinsky et al. 2025) and NGC 4214 (J. L. Carlin et al. 2021). Closed red stars indicate NGC 55 satellites. The red rectangle outlines the parameter space that was tested in artificial dwarf simulations (Section 4). The light blue-shaded region indicates where our dwarf search is ≳80% complete, and the yellow-shaded region indicates where our search is ≲80% complete. Completenesses in these regions outside of the red rectangle are extrapolated. The gray-shaded region indicates where we cannot extrapolate our completeness. Gray-dashed lines indicate lines of constant surface brightness.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: The DELVE-DEEP color–magnitude diagram of our 2-vote candidates (top: Candidate 1, bottom: Candidate 2) and their i-band images. RGB stars are shown in red, stars outside of our RGB selection region are shown in blue, and all other sources are shown in brown. The black line represents an old, metal-poor isochrone (age = 10 Gyr, [Fe/H] = −2, A. Dotter et al. 2008) at the distance of NGC 55. The left panel includes only the sources within a radius of 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 surrounding the candidate, indicated by the red circle in the middle panel. The corresponding detection method is given in the title. The right panel highlights each source from the left panel on the i-band image.
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Average completeness in g and i bands across all 26 coadds used for the artificial star injections. Solid lines indicate mean completeness and shaded regions indicate ±1σ. Average 50% completeness is 25.8  ±  0.2 mag in g and 25.0  ±  0.2 mag in i. TRGB apparent magnitudes in g and i given by blue- and red-dashed lines, respectively (﹩{m}_{g}^{{\rm{TRGB}}}\sim 24.3﹩; ﹩{m}_{i}^{{\rm{TRGB}}}\sim 22.6﹩).
Paper: DELVE-DEEP Survey: The Faint Satellite System of NGC 55
Authors: Jonah Medoff, Burçin Mutlu-Pakdil, Jeffrey L. Carlin, Alex Drlica-Wagner, Erik J. Tollerud, Amandine Doliva-Dolinsky, David J. Sand, Clara E. Martínez-Vázquez, Guy S. Stringfellow, William Cerny, Denija Crnojević, Peter S. Ferguson, Catherine E. Fielder, Astha Chaturvedi, Nitya Kallivayalil, Noelia E. D. Noël, Kathy Vivas, Alistair R. Walker, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Yumi Choi, Gustavo E. Medina, Mahdieh Navabi, Andrew B. Pace, Alex H. Riley, Joanna D. Sakowska
Figure caption: Follow-up Gemini data for Candidate 1. Left: Deep color–magnitude diagram of the region within a 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 radius of the candidate. Isochrone with age = 10 Gyr and metallicity [Fe/H] = −2 at the distance of NGC 55 is shown in red (A. Dotter et al. 2008). Middle: Same as left but for a background region of equal area. Right: An i-band image with a dashed red circle of a radius 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 surrounding the candidate.
Paper: Flat Circular Velocities on a Megaparsec Scale from the ΛCDM Model
Authors: Antonino Del Popolo, Man Ho Chan
Figure caption: Comparison of the rotational curves in Figure 2 of T. Mistele et al. (2024a) with the pISO rotational curves with the described virial radius and concentration. The error bars and shaded band indicate the statistical errors and systematic errors, respectively.
Paper: Flat Circular Velocities on a Megaparsec Scale from the ΛCDM Model
Authors: Antonino Del Popolo, Man Ho Chan
Figure caption: Comparison of the rotational curves in Figure 2 of T. Mistele et al. (2024a) with the NFW rotational curves with the described virial radius and concentration. The error bars and shaded band indicate the statistical errors and systematic errors, respectively.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: (a) The V, X-ray, and gamma-ray light curves of the 2018 outburst of V392 Per against logarithmic time. We assume that the outburst day is tOB = JD 2458236.2 (= UT 2018 April 27.7). The V data are taken from the Variable Star Observers League of Japan (VSOLJ), the American Association of Variable Star Observers (AAVSO), and U. Munari et al. (2020). The Swift X-ray (0.3–10.0 keV) count rates are also added, taken from the Swift website (P. A. Evans et al. 2009). We also add the 0.3–100 GeV gamma-ray flux detected with the Fermi/Large Area Telescope (A. Albert et al. 2022). The large green plus (+) symbols indicate the assumed 0 mag (peak, labeled 0), 2 mag (2), and 3 mag (3) decay from the peak. (b) Same as panel (a), but we overplot our model light curves for a distance modulus in the V band of (m − M)V = 14.6. We assume a Roche lobe–filling companion star with a photospheric temperature of Tph,2 = 6100 K and mass of M2 = 1.0 M⊙. The black line is our free–free + photospheric blackbody model light curve of a 1.37 M⊙ white dwarf (WD). Including the brightnesses of the disk and companion star irradiated by the hot WD and viscous heating of the disk, we plot the thick orange, magenta, cyan, red, and gray lines of our model V light curves for the 1.37 M⊙ WD (Ne3) with the different mass accretion rates in Table 1. The thin colored lines are for the corresponding model X-ray fluxes (0.3–10.0 keV), although the thin red and gray lines are overlapped. The yellow arrows indicate the path in which we reduce ﹩-{\dot{M}}_{2}=1.7\times 1{0}^{-7}﹩ to 1.0 × 10−9 M⊙ yr−1.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Theoretical maximum V magnitude vs. rate of decline (MMRD) diagram: (a) ﹩\mathrm{log}({t}_{3})﹩–MV,max and (b) ﹩\mathrm{log}({t}_{2})﹩–MV,max. The blue lines indicate the model equi-WD mass lines, from left to right, 1.35, 1.3, 1.25, 1.2, 1.1, 1.0, 0.9, 0.8, 0.7, and 0.6 M⊙; the thick solid gray lines denote the model equi-mass accretion rate (﹩{\dot{M}}_{{\rm{acc}}}﹩) lines, from bottom to top, 3 × 10−8, 1 × 10−8, 5 × 10−9, 3 × 10−9, 1 × 10−9, 1 × 10−10, and 1 × 10−11 M⊙ yr−1; and the red lines represent the model equi-recurrence time lines, from bottom to top, trec = 30, 100, 300, 1000, 10,000, 105, 106, and 107 yr. These lines are taken from I. Hachisu et al. (2020) based on the optically thick nova wind model (M. Kato & I. Hachisu 1994) and nuclear runaway model calculation of mass accretion onto each WD. The thick yellow line corresponds to the x0 = 2 line, below which the models are not valid (see I. Hachisu et al. 2020 for details). We overplot V392 Per (filled blue square), filled red circles taken from the “golden sample” of B. E. Schaefer (2018), filled stars taken from P. Selvelli & R. Gilmozzi (2019), and an open star (V1500 Cyg) taken from M. della Valle & L. Izzo (2020). We further add two novae, KT Eri (open blue triangle, I. Hachisu et al. 2025) and V339 Del (open blue square, I. Hachisu et al. 2024). In panel (a), the thick solid black line indicates the empirical line for the MMRD relation obtained by P. Selvelli & R. Gilmozzi (2019). In panel (b), the thick solid cyan line represents the empirical MMRD line obtained by M. della Valle & L. Izzo (2020).
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: The B, V, and IC light curves of V392 Per against logarithmic time. We shift up B by 0.8 mag but shift down IC by 1.5 mag. The BVIC data are all taken from AAVSO. The three light curves decay similarly. The thin solid black line labeled “free–free” denotes our FF+BB model light curve of the 1.37 M⊙ WD (Ne3). The magenta (labeled “irradiated disk”) and orange+yellow (labeled “viscous heating disk”) lines denote our model V light curve of the magenta line in Figure 2(b), but the magenta part is dominated by the irradiated disk and the orange+yellow part is dominated by the viscous heating disk. The purple line denotes the soft X-ray flux, which is the same as the magenta line in Figure 2(b).
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: (a) The B, V, and IC light curves of the 2018 outburst of V392 Per against logarithmic time. We assume that the outburst day is tOB = JD 2458236.2 (= UT 2018 April 27.7). (b) The 2009 outburst of KT Eri. The data are the same as those in I. Hachisu et al. (2025). (c) The 2013 outburst of V339 Del. The data are the same as those in I. Hachisu et al. (2024).
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Same as Figure 2(b), but for a photospheric temperature of the companion star of (a) Tph,2 = 4500 K or (b) Tph,2 = 3500 K. The other symbols are the same as those in Figure 2(b).