adsabs/AstroCLIMB huggingface dataset:
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: Median stacked images of the Type-0 subsample in the u* to MIPS 24 μm bands. The red circles indicate the bands where we find a stacked flux with S/N > 2.
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: The best-fit SED and the probability distribution functions of the derived parameters of an example galaxy in our sample performed using the whole available photometry (left) and without the 350 and 500 μm (right).
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: Distribution of the photometric redshifts of the individual sources in this work (crimson) compared with the results of T21 (teal blue) for their similarly defined primary samples.
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: Redshift distribution of the 76 sources in the primary sample with a counterpart in the COSMOS2020 catalog: in green we show the redshifts computed in this work; in red the redshifts reported in the COSMOS2020 catalog.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Entropy slices at 1.76 s post-bounce for the 40 M ⊙ solar-metallicity progenitor in the z - x, z - y, and y - x planes. The black circle shows the position of the central object, while the arrows show the projected kick velocity directions. Note the very asymmetric morphology (most notable in the y - x plane) and ongoing significant infall accretion (most notable in the z - y plane, at “five o’clock”). The two high-entropy jets originating from the central compact object and their complicated cocoon structures are clearly in evidence (in red). The inner blue/light-blue interface is the neon/oxygen interface in the progenitor. See discussion in Sections 4 and 7.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: 3D volume rendering of the explosion at 1.76 s after bounce showing the entropy, Y  e , and density of the central region. The viewing directions in all panels except the bottom right one are the same as in Figure 11, which is perpendicular to the general direction of the neutrino-driven jets. The viewing direction of the bottom right panel is along the jets. Top left: entropy distribution in the central region. At this time, the high-entropy material moves out only along the jets. Top right: electron fraction distribution in the central region. A jet and disk structure can be seen, in which the jets are proton-rich (Y  e  > 0.5; orange red) and the disk is neutron-rich (Y  e  < 0.5; blue). For this rendering, the Y  e  = 0.5 region is made more translucent. Bottom left: density distribution in the central region with the same orientation as above. Only matter with ρ > 107 g cm−3 is shown here. The higher-density matter roughly traces the shape of the disk. Bottom right: same as the bottom left panel, but as viewed down the axis of the top right jet.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: 3D volume rendering of the explosion at 1.76 s after bounce and on a large scale. At this time the shock wave has achieved a distance of ∼20,000 km. The viewing angles in the two panels are perpendicular to each other. Color shows the entropy, and the black circles shows the position of the PNS that will very soon transition to a black hole. The explosion is very asymmetrical, and two high-entropy jets originating from the central compact object are clearly seen (in red).
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Top: maximum shock radii (in kilometers) as a function of time after bounce (in seconds) for a collection of 3D models. The black lines trace the evolution of the two models shown here (the 12.25 and 14 M ⊙ ZAMS progenitors) that do not explode by the neutrino mechanism and are destined to form black holes. Note that the maximum shock radius for the 40 M ⊙ model first decreases and then starts to experience a combination of the SASI and spiral SASI over a period of ∼100 ms before and as it explodes. Bottom: a close-up of the left panel provided to focus in on the spiral SASI-like oscillations as seen via the motion of the shock radius for the three models shown here that form black holes, though by two different mechanisms. The SASI class oscillations for the two nonexploding black hole formers can be seen starting near ∼0.4 s and continue thereafter. See the text for a discussion.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Angle-averaged neutrino luminosities in the observer frame for the ν  e , ﹩{\bar{\nu }}_{e}﹩, and “ν  μ ” species at 500 km as a function of time after bounce. The 40 M ⊙ model shows the aforementioned outlier behavior, with its significantly higher neutrino luminosity for all species, corresponding to its higher compactness and accretion rate. The black lines are for the 12.25 and 14 M ⊙ black hole formers.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Gravitational-wave strain for both + (top) and × (bottom) polarizations as a function of time after bounce (in seconds) for two representative 3D models (the 9b and 23 M ⊙), in comparison with the corresponding strains for the 40 M ⊙ model. This reflects a hierarchy in initial model compactness. Note the greater magnitude of the strain and memory (offset from zero) for the latter.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Here we plot the mean lapse radial profiles at 0.01 s after bounce and 1.75 s after bounce for our 3D 9b, 23, and 40 M ⊙ models. Notice how much more deeply the 40 M ⊙ profile plunges, achieving a value in the center of ∼0.35 at the time of black hole formation (∼1.76 s after bounce). See text for a discussion.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Entropy map before (top) and during (middle and bottom) the excitation of the SASI/spiral SASI mode.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Gravitational-wave energy radiated (in M ⊙ c2) from matter (left) and neutrinos (right) as a function of time after bounce (in seconds) for many comparison 3D models vis à vis the 40 M ⊙ model.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: The [C II]/FIR ratio plotted as a function of FIR surface brightness (ΣFIR). The points are color coded according to their region. The comparison data are from NGC 7331 (Sutter & Fadda 2022), star-forming regions in local galaxies from galaxies in the KINGFISH survey (Sutter et al. 2019), z ∼ 0.02–0.2 galaxies from Ibar et al. (2015), and local U/LIRGS from the GOALS survey (Díaz-Santos et al. 2017). The central gray line corresponds to the linear fit of the comparison points, while the lines limiting the blue-shaded region correspond to 5 times the dispersion of the positive and negative residuals. Such a region contains points where the [C II] emission is powered by star formation. Points higher than the upper line have an excess of [C II] emission.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Kennicutt–Schmidt diagram of the different regions in Arp 25. The values from NGC 7331, a Milky Way analog from Sutter & Fadda (2022), and the band defined in Bigiel et al. (2008) for subkiloparsec regions in galaxies are plotted for comparison. The cross shows the typical error bars for the measured values of Arp 25.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: The 12CO1→0/FIR values plotted against the [C II]/FIR values of the apertures in Arp 25 over a grid of PDR models of Kaufman et al. (2006) (available in the PDR toolbox; see Pound & Wolfire 2023). The region populated by normal galaxies is shaded in blue. For comparison, we plotted data from regions of the Milky Way analog NGC 7331 (Sutter & Fadda 2022) and normal star-forming galaxies from Hughes et al. (2017) and Gullberg et al. (2015).
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Surface brightness of the [C II] line plotted as a function of the attenuated UV light determined using the CIGALE SED fits. Arp 25 data are color coded based on their regions. Comparison data from the nearby galaxy NGC 7331 and M31 are shown as gray and purple symbols, respectively. A linear fit of the relationship using the NGC 7331 and M31 and the 3σ region are shown shaded in light blue.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: The ratio of the 7.7 and 11.3 μm PAH feature fluxes vs. [C II] to PAH ratio. The PAH7.7μm/PAH11.3 μm ratio is indicative of the average charge of the PAHs. The histograms on the top and side show the distribution of the comparison samples shaded in gray and the data from Arp 25 outlined in yellow.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Relation between the radius and mass of the envelope for the SNe IIb progenitor models (blue dots) generated by Ouchi & Maeda (2017). The analytical relation derived by Ouchi & Maeda (2017) that explains the properties of the numerical evolution models is shown by the black line. Also shown here are the possible combinations of the radius and envelope mass of SN 2022crv (red dots) generated from the semi-analytical model of Nagy & Vinkó (2016); note that the radius here is an upper limit for a given mass, and therefore the blue shaded area is the allowed region for SN 2022crv.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Bolometric light curve of SN 2022crv is plotted along with the fit with the toy model of Valenti et al. (2008a). The best fit from the two-component semi-analytical model proposed by Nagy & Vinkó (2016) is also shown along with the contribution from the individual core and shell components.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Optical color evolution of SN 2022crv compared to a sample of SE-SNe. The SE-SNe sample has been corrected for Milky Way and host galaxy extinction. The templates from Stritzinger et al. (2018) are also overplotted. The blue-colored points are for SNe IIb, and the red-colored points are for SNe Ib. The data for the comparison sample are taken from the papers cited in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Peak spectral luminosities vs. time to peak for some well-observed CCSNe from the literature (Bietenholz et al. 2021, and references therein). The position of SN 2022crv is denoted as per the 5.5 GHz light curve. The dotted lines represent the mean velocities of radio-emitting shells in an SSA scenario with p = 3.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Upper panel: Radio light curves of SN 2022crv at 0.44, 0.69, 1.37, 5.5, and 9.0 GHz. The down-pointing triangles are the upper limits of the flux densities. Lower panel: Near-simultaneous spectral indices between 9/5.5 GHz (red circles) and 1.4/0.7 GHz (green circles).
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Radio light curves of SN 2022crv at frequencies ν = 0.69–9 GHz. The solid red curves represent the best-fit SSA model. The filled black circles denote the observed flux densities.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption:  BVRI bolometric light curve of SN 2022crv generated using SuperBol. The bolometric light curves of all the comparison objects are also calculated using SuperBol using the values computed in Table 1.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Radius and temperature evolution of SN 2022crv up to +86 days. The radii and temperatures are estimated under the blackbody approximation.
Paper: Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a Very Thin Hydrogen Envelope
Authors: Anjasha Gangopadhyay, Keiichi Maeda, Avinash Singh, Nayana A. J., Tatsuya Nakaoka, Koji S. Kawabata, Kenta Taguchi, Mridweeka Singh, Poonam Chandra, Stuart D. Ryder, Raya Dastidar, Masayuki Yamanaka, Miho Kawabata, Rami Z. E. Alsaberi, Naveen Dukiya, Rishabh Singh Teja, Bhavya Ailawadhi, Anirban Dutta, D. K. Sahu, Takashi J. Moriya, Kuntal Misra, Masaomi Tanaka, Roger Chevalier, Nozomu Tominaga, Kohki Uno, Ryo Imazawa, Taisei Hamada, Tomoya Hori, Keisuke Isogai
Figure caption: Peak absolute magnitude vs. Δm 15 of SN 2022crv in comparison with a sample of SNe IIb and SNe Ib from Taddia et al. (2018) and Table 1.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: A selection of historical bursts in EX Lup. The three figures in the first row show EX Lup’s historical outbursts in 1945, 1955, and 2008. The 1945 outburst is additionally fitted with a spline in red. The figures in the second and third rows show the characteristic bursts. The blue points are B-band magnitudes from DASCH light curves. The open circles are visual photometry from Albert Jones and are transformed to the Johnson V band via Equation (1). The black points are transformed by AAVSO visual magnitude, and the black crosses are photometry made in the Johnson V band from AAVSO. Red points denote the SMARTS V-band light curves. The equivalent mass accretion rates derived from excess emission relation are displayed on the right axes. The estimated accreted mass M acc,b during each burst and its ratio to the quiescent accretion M acc,q with the same duration is displayed on the upper right in each panel. The red dashed line represents the V-magnitude baseline for the mean quiescent rate (1.7 × 10−9 M ⊙ yr−1). The blue dashed line represents the V-band fluxes of EX Lup’s photosphere.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: A schematic illustration of a two-component spot model that can produce the observed multicolor light curves. (a) The multicolor light curves from the two-component spot model. The predicted phase lags between U and other bands are indicated. (b) The intensity plot of the stellar surface for the two-component spot model, with hot (blue) and cool (dark red) spots, and uniform photosphere background (red). The adopted model parameters are listed in Table 6. (c) The phase shift and morphological change of synthetic I-band light curves according to different longitude differences of two spots ΔΩ. (d) The resulting phase lags of brightness maxima between U- and I-band light curves as a function of spots’ longitude differences. This set of figures is produced by the python package starry (Luger et al. 2019).
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Comparisons of EX Lup VLT/X-Shooter spectrum with best-fit extinction A  V  for three photosphere templates. The photosphere templates are taken from the non-accreting YSOs’ VLT/X-Shooter spectra of Manara et al. (2013), with names and spectral types indicated on the upper left. We assume A  V  = 0 for these photosphere templates. The best-fit A  V  for each template is obtained by minimizing the standard deviation (listed lower left) of accretion fluxes (red) between 4000 and 6000 Å and is also displayed on the upper right. The EX Lup spectrum (gray) is dereddened with best-fit A  V  in each panel. The templates are added with constant fluxes (black) to compare with EX Lup spectrum.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The histogram of accreted masses M acc of 10 bursts from Figure 14. The black sticks at the bottom mark the value of M acc for each burst. The error bars of the number of bursts in each M acc bin are the Poisson error due to the small sample size. The dashed line is a power-law relation fitted to the burst number in the three accreted masses bins. However, the K-S test suggests the accreted mass of 10 bursts is not likely sampled from such power-law distribution (with a p-value of 1.08 × 10−5), due to the non-detections between 10−8.0 ∼ 10−7.25 M ⊙.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: An overview of less characterized bursts seen from EX Lup. The photometry symbol scheme is the same as Figure 14. These bursts are hard to have robust accreted masses estimates, either due to incomplete photometry coverage caused by seasonal observational gaps or inconsistent data reported by different observers.