adsabs/AstroCLIMB huggingface dataset:
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: We select quiescent galaxies by the relative difference, ﹩{\rm{\Delta }}\,{\mathrm{log}}_{10}({\rm{SFR}\,}_{\,\rm{SFMS}})﹩, between their ﹩{\mathrm{log}}_{10}({\,\rm{SFR}\,}_{100})﹩ and the SFMS at their redshift from J. Leja et al. (2022) as a function of stellar mass. Quiescent galaxies are selected to be at least 0.5 dex below (dotted line) the main sequence of star-forming galaxies from J. Leja et al. (2022; solid curve). Quiescent galaxies in the protocluster and in the field are shown as red stars and purple crosses, respectively. We find a total of 217 protocluster members (34 quiescent galaxies) and 216 field members (29 quiescent galaxies). As shown in the histograms in the top and right panels, we find that the two subsamples are distributed similarly.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: Wind-momentum–luminosity relation at SMC metallicity expressed in cgs units. Gray points mark empirical results, with ﹩\dot{M}﹩ obtained from Hα or combined optical–UV analyses (P. Massey et al. 2004, 2005, 2009; S. R. Heap et al. 2006; M. R. Mokiem et al. 2006, 2007; J. C. Bouret et al. 2013). When these works considered clumping, we computed the equivalent smooth-wind mass-loss rate (﹩{\dot{M}}_{\mathrm{smooth}}=\dot{M}/\sqrt{{f}_{\mathrm{vol}}}﹩, with fvol being the clumping volume filling factor; see, e.g., J. Puls et al. 2008, Sect. 6.3) prior to calculating the wind-momentum rate. Hα only provides upper limits for mass-loss rates at ﹩{\mathrm{log}}\,{L}_{* }/{L}_{\odot }﹩ ≲ 5.2–5.4 (downward triangles). We note the change of slope between the high-luminosity objects and the less-luminous ones at this L*. The gray lines represent the theoretical WLR derived by J. S. Vink et al. (2001; solid) and scaled to the SMC metallicity and more modern relations at SMC metallicity by J. Krtička & J. Kubát (2018; dashed–dotted) and R. Björklund et al. (2021; dashed). The shaded region below the yellow line marks the parameter space where Brα is predicted to exhibit narrow emission. Blue and green symbols denote project targets expected to show broad and narrow Brα emission, respectively, while the red sources lie in the expected thin wind regime (see Table 1 for the stellar parameters used in this plot). For some project sources, only upper limits of ﹩\dot{M}﹩ could be constrained by previous works (red downward arrows). Objects with underlined designations have been analyzed in Section 5.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: Left: the quiescent fraction for galaxies in the protocluster (red), combined field (purple), lower-redshift field (light gray), and higher-redshift field (dark gray). The quenched fractions in the protocluster are indistinguishable from the field at high mass (triangles). The quenched fractions in the intermediate-mass (squares) and low-mass (stars) bins are slightly elevated in the protocluster but within ∼2σ of those in the field. Right: the QFE for protoclusters in our work and the current literature around cosmic noon. The current literature has primarily investigated the high-mass regime, with our work extending down to low masses. We have differentiated the stellar mass regimes of the QFE by their shapes if applicable. We note that the QFE from I. McConachie et al. (2022; yellow) includes the ultrahigh-mass galaxies (log(M⋆/M⊙) > 11.0) and are shown as a circle. We also note that half of the sample from K. Ito et al. (2023; blue) also contains ultrahigh-mass galaxies and may be driving the elevated QFE. Lastly, the work of M. Ando et al. (2020; brown) combines several protoclusters from redshift 1.5 to 3.0 across the intermediate- and high-mass bins. Our analysis is consistent with other studies within 2σ, especially in the similar stellar mass bins, and suggests a relatively low excess in quiescent galaxies.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: UVJ color–color diagram in the three stellar mass bins. Similarly to Figure 2, red stars indicate quiescent galaxies in the protocluster, purple crosses indicate quiescent galaxies in the field, and the gray points indicate all other galaxies in the protocluster or field. The solid lines indicate the traditional quiescent wedge from K. E. Whitaker et al. (2011), and the dashed line indicates the S. Belli et al. (2019) selection. We find that all low-mass galaxies would otherwise not be selected using the UVJ diagram. There is significant overlap between quiescent galaxies in the protocluster and field, suggesting that they have similar stellar population properties.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: JWST observations of AzV 446 and archival optical and UV data (black), together with model fits that account for instrumental and rotational/macroturbulence broadening. The best-fitting CMFGEN model (red) reproduces Teff and ﹩{\mathrm{log}}﹩ g diagnostic lines in the visible, as well as classical mass-loss rate indicators in the UV and optical ranges. The model spectra successfully reproduce the observed ﹩\dot{M}﹩-sensitive lines in the L-band (lowermost row). For comparison, the figure includes synthetic spectra for models without clumping (orange) and without X-rays (blue). Such differences in the simulations do not produce any effect on the displayed L-band lines.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: Brα spectra of slowly rotating sample stars, arranged by spectral type and luminosity class. The spectra are shown in the same vertical scale, offset by a constant for clarity. “B,” “N,” and “T” specify the expected regime. Vertical lines mark H I (red), He I (blue), and He II (orange) transitions. Stark absorption wings underlying the Brα emission are absent in AzV 15 and then evolve toward strong absorption in the later types.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: Line fits to a subset of five sample stars, encompassing different wind regimes, with CMFGEN (blue) and FASTWIND (orange) models. The mass-loss rate values obtained by the analysis with CMFGEN are provided next to each star.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: Same as Figure 3, now for the sample stars with ﹩v\sin i﹩ ≥ 150 km s−1. The high rotational velocities broaden the Brα profiles and cause the apparent disagreement between observations and the prediction. The late spectral types show the broad absorption wings seen in Figure 3, although somehow washed out by the fast rotation.
Paper: Probing Thin Winds in Massive OB Stars of the SMC with JWST/NIRSPEC Brα Spectroscopy
Authors: Miriam Garcia, Alexander W. Fullerton, Francisco Najarro, Joachim Puls, Daniel J. Lennon, Jean-Claude Bouret, Christopher J. Evans, Margaret Hanson, Artemio Herrero, D. John Hillier, Alexandre Legault, María del Mar Rubio-Díez, Sergio Simón-Díaz, Jon O. Sundqvist, Frank Tramper
Figure caption: Left: NIRSpec spectrum of NGC 346-ELS-090, embedded in intense H II emission, after reduction with and without background subtraction. Right: same, now showing a target within negligible nebulosity.
Paper: Peekaboo: Secular Resonances from Evolving Stellar Oblateness Impede Transit Detections
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Malena Rice, Jack Lubin
Figure caption: Overview of the effects of J2 on transit probability for the outer planets in Kepler-619. The probability that the outer two observed planets transit together when viewed from a random angle (irrespective of whether the inner planet transits at this angle) is shown for 2000 integrations of orbital parameters as a function of initial stellar J2. The inclination distribution for these integrations used a Rayleigh sigma of σi = 0.08 rad ≈ 4﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8. The purple curve represents the mean probability as a function of J2.
Paper: Peekaboo: Secular Resonances from Evolving Stellar Oblateness Impede Transit Detections
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Malena Rice, Jack Lubin
Figure caption: (Top) Qualitative schematic of impact-parameter geometry before and after sweeping resonance. Angles, distances, and radii are not to scale. (Bottom) Time evolution of the inclinations of the Kepler-619 system with high initial J2. The inner, middle, and outer planets were initialized with inclinations of 10﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3, 6﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1, and 4﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5; eccentricities of 0.010, 0.006, and 0.0125; and longitudes of ascending node of 1.8, 3.1, and 4.9 rad, respectively. These initial conditions were chosen from the Monte Carlo described in Section 3 and therefore, were chosen arbitrarily to demonstrate clearly what resonance-induced misalignments look like as functions of time.
Paper: Peekaboo: Secular Resonances from Evolving Stellar Oblateness Impede Transit Detections
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Malena Rice, Jack Lubin
Figure caption: Overview of the effects of J2 on average transit probability for the planets in Kepler-619 over a Monte Carlo of 2000. Longitudes of ascending node were assigned uniformly, and inclinations were drawn from a Rayleigh distribution with σi = 0.08 ≈ 4﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5. The blue, orange, and green lines represent the probabilities that exactly one, two, or three planets transit, respectively. The red dashed line represents the probability that two or more planets transit, and the purple dashed line represents the probability that the outer two planets transit. Overall, at high J2 values, the system is more likely to be seen as a single-transiting system and less likely with two or more transiting planets, despite the outer two planets cotransiting more commonly at high J2 values.
Paper: Peekaboo: Secular Resonances from Evolving Stellar Oblateness Impede Transit Detections
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Malena Rice, Jack Lubin
Figure caption: Ratios of transit probabilities between initial J2 values of 10−3 and 10−5 as a function of the Rayleigh distribution σi for the initial inclination distribution for Kepler-619. The blue, orange, and green lines represent the probabilities that exactly one, two, or three planets transit, respectively. The red dashed line represents the probability that two or more planets transit, and the purple dashed line represents the probability that the outer two planets transit (irrespective of the inner). To account for the breadth of potential models describing the intrinsic inclination distribution of exoplanet systems, we display each case out to large Rayleigh distribution widths σi (see Section 4 for more details).
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: PSF-subtracted MUSE image of AB Aurigae constructed from the average of the 6558.88 Å and 6560.13 Å slices (i.e., slightly blueshifted from Hα) from OB4, showing a clear detection of AB Aurigae b at ≈0﹩\mathop{.}\limits^{^{\prime\prime} }﹩6 slightly counterclockwise of due south. The region within 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩3 is masked for clarity because it is heavily affected by saturated/nonlinear pixels, especially in some channels centered on the Hα line.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Reference spectrum subtraction of the Hα data slightly redshifted from the Hα line center (6563.88–6565.13 Å) where AB Aur b’s signal is clearly visible and at the Hα line center (6562.63 Å; bottom) where it is marginally detectable. Note that the color intensity scaling is reversed compared to prior figures. For clarity, the yellow arrow points to the location of AB Aur b’s emission in the blueshifted channels. The bright region along the image’s center right is a residual detector striping artifact caused by saturation.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Other MUSE reductions showing the detection of AB Aur b from OB4. (Left and middle) 6558.88 Å and 6560.13 Å from the reduction shown in Figure 1. Average of the 6558.88 Å and 6560.13 Å slices from a classical SDI reduction (right). In each panel, we mask the field out to a separation affected by horizontal striping and saturation.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: The AB Aurigae primary’s spectrum over the entire MUSE wavelength range, with an inset showing the full Hα region, including the absorption component (top), and focused on the Hα emission line.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Subtraction of the blueshifted Hα data from Figure 1 by the MCMC model corresponding to the median of the posterior distributions. The inset shows the MCMC model with the same color intensity scaling.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Subtraction of the redshifted Hα data from Figure 4 (bottom panel) by the MCMC model corresponding to the median of the posterior distributions. The inset shows the MCMC model with the same color intensity scaling.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Detection of AB Aur b from OB2 (left and middle panels) and weaker detection from OB1 in blueshifted Hα (right).
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: CHARIS total intensity wavelength-collapsed image (T. Currie et al. 2022; T. Currie 2024) and polarized intensity image (E. Dykes et al. 2024) with MUSE contours (magenta) overplotted at intensities of 1250 and −2500 × 10−20 erg s−1 cm−2 Å for the blueshifted and redshifted channels, respectively. The horizontal shaded region identifies where MUSE data are affected by horizontal striping artifacts and (for ρ ≲ 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩3) nonlinearity and saturation. AB Aur b is the only signal clearly detected with MUSE at SNR > 5 and colocated with a feature seen with CHARIS. Bright regions at smaller separations (ρ ≲ 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩3) are affected by detector nonlinearity and residual striping: they do not clearly trace any extended feature, and the significance of their detections using standard high-contrast imaging metrics described in the main text (T. Currie et al. 2011; D. Mawet et al. 2014) is SNR ≲ 2.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: (Left) Spectrum of AB Aur b compared to scaled stellar spectra for OB4 and OB2. The corresponding velocities are in the system rest frame and are corrected for the system’s radial velocity (Gaia Collaboration et al. 2023). We obtain consistent AB Aur b spectra from an alternate extraction, treating the position and spatial extent of AB Aur b as free parameters for each channel instead of fixing them to results obtained in Section 5.1. (Right) Spectrum of AB Aur b compared to the average spectrum of the disk at two angular separations and within one spiral arm.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: (Top left) PSF-subtracted MUSE image of AB Aurigae constructed from the average of the 6558.88 Å and 6560.13 Å slices in OB4 using a second-degree polynomial fit instead. (Top right) The difference between this image and the one presented in Figure 1. (Bottom panels) The results shown for redshifted wavelengths showing AB Aur b in absorption. Note the difference in the intensity scale for the difference images (right-hand panels).
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Spectrum of AB Aur b compared to that of the protoplanets PDS 70 b and c and the accreting T Tauri star V345 Mon. The VAMPIRES Hα bandpass used for a detection of AB Aur b in T. Currie et al. (2022) covers ≈6558–6568 Å; the HST/WFC3 Hα bandpass (F656N) used for AB Aur b’s detection (Y. Zhou et al. 2022; B. P. Bowler et al. 2025) covers ≈6552.5–6570.4 Å.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: (Top panels) Raw (pre-PSF subtraction) OB4 MUSE image at blueshifted and redshifted wavelengths. (Bottom left) Azimuthally averaged radial intensity profile for the blue- and redshifted channels. (Bottom right) Raw spectrum at the location of AB Aur b in OB4 normalized to the median intensity value across the entire wavelength range.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: VLT/MUSE Hα image (left) and extracted spectra (right) for PDS 70 bc from data originally published in S. Y. Haffert et al. (2019) and also reduced in J. Hashimoto et al. (2020).
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: The same as Figure 11 except for differences in the range of wavelengths masked when constructing the reference spectrum.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Corner plot showing the posterior distributions estimated from emcee for AB Aur b in blueshifted Hα.
Paper: VLT/MUSE Detection of the AB Aurigae b Protoplanet with Hα Spectroscopy
Authors: Thayne Currie, Jun Hashimoto, Yuhiko Aoyama, Ruobing Dong, Misato Fukagawa, Takayuki Muto, Erica Dykes, Mona El Morsy, Motohide Tamura
Figure caption: Corner plot showing the posterior distributions estimated from emcee for AB Aur b in redshifted Hα.
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: (Top panel) The temporal evolution of the temperature for the hot and cool components of SN 2023xgo. Blue symbols denote the hot component from the single-blackbody model. Green symbols denote the hot component, and orange symbols denote the cold component, both from the combined model. Red symbols denote the cold component from the single dust model. Blue, green, and orange symbols represent values obtained using g-, r-, o-, J-, H-, and Ks-band data. Red circles, on the other hand, denote those obtained using J-, H-, and Ks-band data. (Bottom panel) The evolution of the dust mass obtained from the SED fitting. Orange filled squares denote the dust mass obtained using g-, r-, o-, J-, H-, and Ks-band data, while red open squares are obtained using J-, H-, and Ks-band data.
Paper: The Near-infrared Echo from SN 2023xgo: Evidence for a Massive Presupernova Eruption in a Type Ibn/Icn Supernova
Authors: Masayuki Yamanaka, Takahiro Nagayama
Figure caption: The JHKs-band absolute magnitude light curves of SN 2023xgo are presented in each panel, showing the absolute magnitudes in the J, H, and Ks bands. The distance modulus and extinction corrections have already been applied. These light curves are compared with those of Type Ibn SNe 2006jc (E. Di Carlo et al. 2008; S. Mattila et al. 2008), 2010al (A. Pastorello et al. 2015a), and OGLE2012SN 006 (A. Pastorello et al. 2015b), as well as a normal SN Ic (D. J. Hunter et al. 2009).