adsabs/AstroCLIMB huggingface dataset:
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: H2O and CO2 spectra convolved to an R of 3000 around the CO2 0110–0000 transition. The top panels show slab-model spectra using parameters that reproduce the observational data (Salyk et al. 2011). The four panels below show the DALI output spectra for the thin-disk structure with 99.9% large, settled grains. The second panel shows the base DALI model, the third base DALI with water UV-shielding, the fourth base DALI with water UV-shielding and extra chemical heating, and the fifth panel shows the same model as the fourth panel, now assuming emission can only originate from the region within the water midplane ice line. The slab models clearly predict a CO2 feature at 15 μm that is weaker than the surrounding water lines, while most DALI models show a brighter CO2 feature compared to the water lines. Only when combining water UV-shielding, extra chemical heating, and a restricted radial emitting region does the thermochemical flux ratio come close to the observed flux ratio as exemplified by the slab models.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: CO2 abundance for the thin model with a large grain fraction of 99.9% for variation in the thermochemical model. The red contour shows the region from which 90% of the CO2 0110–0000 R(20) emission line originates, the yellow contour shows the region from which 90% of the H2O 113,9–100,10 line flux at 17.2 μm originates, the orange line shows the continuum τ 15μm = 1 surface, and the vertical yellow and red bands show the locations of the H2O (0.4  au) and CO2 (1.2 au) midplane ice lines, respectively.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: Gas temperature as a function of the cumulative vertical CO2 column at the location of the midplane H2O ice line (0.4 au). The CO2 column is a proxy for the location in the disk, with higher column being deeper into the disk. In the base DALI model, CO2 is present at a significant abundance over most of the vertical extent of the molecular layer and so the CO2 temperature changes continuously with increasing CO2 column or increasing depth. In the heating and shielding model, after reaching a column of about 1016 cm−2 at a temperature of 600 K, the CO2 abundance drops significantly. Only very deep into the disk when the temperature has dropped down to 200 K does the CO2 abundance reach appreciable levels and the vertical CO2 column increase again with depth. This causes the strong jump in the temperature profile.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: Normalized spectra convolved to R = 3000 for the chemical heating model with (solid) and without (dashed) water UV-shielding assuming a thin structure with a surface layer gas-to-dust ratio of 105. CO2 is assumed to only be present within the water midplane radius for all these models. The top panel shows 12CO2 and 13CO2 in red and purple, respectively. The bottom panel shows the combined spectra. Spectra have been normalizing to the 12CO2 0110–0000 Q-branch peak and are zoomed in on three regions with Q branches of interest. While the individual 0110–0000 P- and R-branch lines show little differences in normalized flux, the various Q-branch features are impacted by the different abundance structures. Ratios between these can thus be used to derive the deeper abundance structure.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: Spectra of OH, CO2, and H2O for the base and H2O UV-shielding and chemical heating models. The emitting region has been constrained to the radial region within the water midplane ice line, and the spectra have been convolved to R = 3000. LTE excitation is assumed for OH.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: As Figure 3 but from the thin model with a surface layer gas-to-dust ratio of 104.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: As Figure 3 but from the thick model with a surface layer gas-to-dust ratio of 104.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: As Figure 3 but from the thick model with surface layer gas-to-dust ratio of 105.
Paper: Constraining High-redshift Stellar-mass Primordial Black Holes with Next-generation Ground-based Gravitational-wave Detectors
Authors: Ken K. Y. Ng, Gabriele Franciolini, Emanuele Berti, Paolo Pani, Antonio Riotto, Salvatore Vitale
Figure caption: Projected upper limit on f PBH as a function of M  c  drawn from the merger rate density measurement in the simulated universe without PBHs and scaled to one year of observations. We also show the current most stringent constraints in this mass range coming from microlensing searches (assuming Poisson initial condition at formation; Gorton & Green 2022; Petač et al. 2022) by MACHO/EROS (E) (Alcock et al. 2001; Allsman et al. 2001) and Icarus (I) (Oguri et al. 2018); measurements of galactic X-rays (Xr) (Manshanden et al. 2019) and X-ray binaries (XRayB) (Inoue & Kusenko 2017); CMB distortions by spherical or disk accretion (Planck S and Planck D, respectively) (Ali-Haïmoud & Kamionkowski 2017; Serpico et al. 2020); and dwarf galaxy heating (DGH) (Lu et al. 2020; Takhistov et al. 2022). LVKC stands for the constraint coming from the LIGO/Virgo/Kagra Collaboration merger rate measurements (Ali-Haïmoud et al. 2017; Raidal et al. 2017; Vaskonen & Veermäe 2020; Franciolini et al. 2022; Wong et al. 2021). We ignore the role of accretion, which has been shown to affect constraints on masses larger than ﹩{ \mathcal O }(10)\,{M}_{\odot }﹩ (De Luca et al. 2020b, 2020c, 2020d). For more details, see the review in Carr et al. (2021). In yellow, we show forecasts for the limits that will be set by microlensing searches with the Rubin observatory (Drlica-Wagner et al. 2019; Bird et al. 2022).
Paper: Constraining High-redshift Stellar-mass Primordial Black Holes with Next-generation Ground-based Gravitational-wave Detectors
Authors: Ken K. Y. Ng, Gabriele Franciolini, Emanuele Berti, Paolo Pani, Antonio Riotto, Salvatore Vitale
Figure caption: Posterior of the merger rate densities of the total mergers (black), PBH mergers (green), and Pop III mergers (red) using phenomenological models (top panel) and Gaussian process regression (bottom panel) in a universe with β PBH = 1/5 (f PBH ≈ 10−4). The darker (light) color band corresponds to 68% (95%) CI. The dashed and solid lines indicate the median of the inferred rate densities and the true rate densities, respectively. Because we cannot model each subpopulation in GPR, there are no posteriors of the merger rate densities of the individual subpopulations.
Paper: Constraining High-redshift Stellar-mass Primordial Black Holes with Next-generation Ground-based Gravitational-wave Detectors
Authors: Ken K. Y. Ng, Gabriele Franciolini, Emanuele Berti, Paolo Pani, Antonio Riotto, Salvatore Vitale
Figure caption: Posteriors of f PBH given (M  c , σ) = (30M ⊙, 0.3) at β PBH = 0, 1/9, 1/5, 1/3, and 1/2. The true values of f PBH corresponding to β PBH are marked by squares in each violin plot. The solid black lines indicate the 95% CIs. The prior is reweighted to be uniform in f PBH.
Paper: Constraining High-redshift Stellar-mass Primordial Black Holes with Next-generation Ground-based Gravitational-wave Detectors
Authors: Ken K. Y. Ng, Gabriele Franciolini, Emanuele Berti, Paolo Pani, Antonio Riotto, Salvatore Vitale
Figure caption: Corner plot of the posteriors of the four hyperparameters (a III, b III, z III, β PBH), for a universe with β PBH = 1/5. 2D contours and black dashed lines represent the 68% and 95% CIs of the marginalized 2D and 1D posteriors, respectively. True values are marked by black solid lines. Dotted lines in the diagonal slots show the uncorrelated priors on the hyperparameters.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications for Carbon Dioxide Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny K. Calahan, Sara E. Duval
Figure caption: CO2 spectra around 4.3 μm convolved to R = 3000. Most flux is produced by the 0001(1)–0000(1) band, but there also is a contribution of the 0111(1)–0110(1) band. The top panel shows the spectra including the full extent of the CO2 emission for base DALI (light blue) and our complete model with H2O UV-shielding and extra chemical heating. The bottom panel shows the same models, but with the CO2 emission constrained to within the H2O midplane ice line. The light gray spectra show the slab model that fits to the observations, using an ﹩{N}_{{\mathrm{CO}}_{2}}=3\times {10}^{15}﹩ cm−2 and T = 700K. In contrast to the 15 μm feature, the thermochemical models, are all significantly weaker than the slab model.
Paper: Viability of Novae as Sources of Galactic Lithium
Authors: Alex J. Kemp, Amanda I. Karakas, Andrew R. Casey, Benoit Côté, Robert G. Izzard, Zara Osborn
Figure caption: Li mass contributions from different sources as a function of Galactic age. See main text for discussion.
Paper: Viability of Novae as Sources of Galactic Lithium
Authors: Alex J. Kemp, Amanda I. Karakas, Andrew R. Casey, Benoit Côté, Robert G. Izzard, Zara Osborn
Figure caption: As Figures 3 and 4 when the common-envelope parameter λ CE is set to 0.5, rather than the Wang et al. (2016) prescription used in our baseline case. This physics case doubles the expected nova rate in M31 (Kemp et al. 2021, and we see this reflected in a doubling in Li production). The ability of observationally derived nova yield profiles to reproduce the protosolar Li abundance, and the inability of theoretical yield profiles, appears robust.
Paper: Viability of Novae as Sources of Galactic Lithium
Authors: Alex J. Kemp, Amanda I. Karakas, Andrew R. Casey, Benoit Côté, Robert G. Izzard, Zara Osborn
Figure caption: Li abundance vs. [Fe/H] in our Galactic models, overlaid with the protosolar Li abundance (Lodders et al. 2009) (yellow cross-hair) and Li abundance data from GALAH DR3 (Buder et al. 2021). All models include AGB, massive stellar, and GCR sources in addition to the designated nova yield set.
Paper: Viability of Novae as Sources of Galactic Lithium
Authors: Alex J. Kemp, Amanda I. Karakas, Andrew R. Casey, Benoit Côté, Robert G. Izzard, Zara Osborn
Figure caption: Delay-time (upper panel, tracking when the nova eruptions occur relative to star formation) and ejecta delay-time (lower panel, tracking when mass is ejected relative to star formation) distributions for Z = 10−3. Both distributions are normalized per solar mass of star-forming material M ⊙SFM (for details, see Kemp et al. 2021, 2022).
Paper: Viability of Novae as Sources of Galactic Lithium
Authors: Alex J. Kemp, Amanda I. Karakas, Andrew R. Casey, Benoit Côté, Robert G. Izzard, Zara Osborn
Figure caption: Observationally derived A(7Be), corrected for 7Be decay since eruption. Decay-corrected A(7Be) values are taken from Molaro et al. (2020) Table 1 (V339 Del, V5668 Sgr, V2944 Oph, V407 Lup, V357 Mus, V906 Car), Molaro et al. (2022) table 4 (V6595 Sgr, V838 Her, V5669 Sgr), and Izzo et al. (2022) (ASASSN-19qv, ASASSN-20ni).
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: Left: the v–r angle distributions for wide binaries at 400–1000 au (blue) and for simulated models (black and red). The best-fit power-law model of α = 2.14 (dotted black) describes well the overall trend of twin binaries (solid blue) but with some noticeable differences. The dashed red line corresponds to 81.1% of normal wide binaries and 18.9% of e = 0.948–0.992 binaries, which agrees with the observation better than the power-law model. Right: the modeled eccentricity distribution (the dashed red line in the left panel) for twin binaries at separations 400–1000 au. The black shaded region shows the 20th–80th percentiles of the model.
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: The power-law indices α of eccentricity distributions (f(e) ∝ e  α ) as a function of binary separations. The black symbols are the results from Hwang et al. (2022) for all binaries, which are dominated by nontwins; the red markers show α and separation bin sizes (horizontal) for the twin binaries. At 100–3000 au, twin binaries are significantly more eccentric (larger α) than other wide binaries at the same separations.
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: The v–r angle distributions for wide binaries with separations at 400–1000 au. The solid and dashed black lines are simulated binaries with arbitrary normalization, showing that circular orbits (solid) have a v–r angle distribution peaking at 90°, and the peaks for eccentric e = 0.9 orbits (dashed) are closer to 0° and 180°. The v–r angle distributions of wide twin binaries (blue) are strongly enhanced at 0° and 180° compared to nontwins (orange), indicating the presence of highly eccentric twins with e > 0.9.
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: The power-law indices α of eccentricity distributions (f(e) ∝ e  α ) as a function of ΔG. Only ΔG < 0.25 mag has a significant increase in α, suggesting that the high eccentricity is specifically associated with the twin excess, instead of a general trend with mass ratios.
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: The distributions of the magnitude difference ΔG among the components of wide binaries at different separations. The vertical dashed line marks ΔG = 0.25 mag, the selection adopted for twin wide binaries in this paper. The distributions are normalized to unity at ΔG = 1.5–2 mag. Compared to binaries at >10,000 au, binaries at separations ≲3000 au show a significant excess of twins at ΔG < 0.25 mag.
Paper: Wide Twin Binaries are Extremely Eccentric: Evidence of Twin Binary Formation in Circumbinary Disks
Authors: Hsiang-Chih Hwang, Kareem El-Badry, Hans-Walter Rix, Chris Hamilton, Yuan-Sen Ting, Nadia L. Zakamska
Figure caption: The posterior distributions of the eccentricity distribution model. The solid lines are the most probable values of the marginalized distributions, and the dashed lines are the highest posterior density interval that includes 64% of the area.
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Light curve of SN 2021aefx from Las Cumbres Observatory (circles), DLT40 (squares), and Swift (stars), offset and binned by 0.01 days for clarity. Phase is given with respect to maximum light in the B band, estimated in Section 3. The left panel highlights the very high-cadence unfiltered light curve from DLT40, with no offset, showing a bump lasting ∼2 days. The middle panel highlights the early Swift photometry, with no offsets, showing an initial decrease in the U and UVW1 filters.(The data used to create this figure are available.)
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Left: fitting the companion-shocking model of Kasen (2010) to the light curve of SN 2021aefx. The solid lines in the top panel show the best-fit SiFTO+Kasen model, with the SiFTO model alone shown with dashed lines. The model reproduces the early optical light curve quite well, but the shock component alone (SiFTO does not extend into the UV) significantly overestimates the early UV flux (bottom). Right: best-fit edge-lit double-detonation model from Polin et al. (2019, solid lines) and nickel-shell model from Magee & Maguire (2020, dotted–dashed lines) compared to the observed light curve (top) and U − B and B − V color curves (bottom) of SN 2021aefx. This double-detonation model is the explosion of a 0.9 M ⊙ WD with a 0.08 M ⊙ helium shell. The model reproduces the early color well but overestimates the absolute magnitude of the bump, while also failing to reproduce the peak absolute magnitude and postpeak colors. The nickel-shell model is a fiducial model of SN 2017cbv plus a shell of 0.02 M ⊙ of 56Ni centered on a mass coordinate of 1.35 M ⊙ with a width of 0.18 M ⊙. This model reproduces the peak better but does not show a strong enough bump in the light curves or color curves.
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Line identification in the premaximum spectra of SN 2021aefx. Colors are a nonlinear function of time; exact phases are listed in Table 1. Our initial spectrum (−16.6 days, dark purple) is dominated by a very broad absorption feature around 570 nm (in the rest frame of the host galaxy). By comparison to later spectra (e.g., at −10 days, dark red), this line likely consists of Si II 597.2 nm, Si II 635.5 nm, and C II 658.0 nm. There may also be a high-velocity (HV) component of Si II 635.5 nm that makes the absorption profile flatter than a Gaussian. The presence of unburned carbon in the early spectrum disfavors the sub-Chandrasekhar-mass double-detonation model for SN 2021aefx.
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Radio data for SN 2021aefx (Kundu et al. 2021) compared to models at various frequencies for a ρ(r) ∝ r −2 wind. Models use ﹩\dot{M}\,=0.96\,(5.0)\,\times \,{10}^{-8}{M}_{\odot }\,{\mathrm{yr}}^{-1}\,({v}_{w}/100\,\mathrm{km}\,{{\rm{s}}}^{-1})﹩ for ϵ  B  = 0.1 (0.01), with solid lines being for ϵ  B  = 0.1. Common parameters in both models are ϵ e = 0.1, T bright = 5 × 1010 K, n = 13 and v  w  = 100 km s−1. The most constraining observation is at 5.5 GHz on day 3.
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Low-resolution spectra of SN 2021aefx. Phases are marked to the right of each spectrum in rest-frame days after the B-band peak. The strongest absorption features in the first spectrum are marked. See Figure 6 for a more detailed view. Telluric wavelengths are marked with the ⊕ symbol.(The data used to create this figure are available.)
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Top: high-resolution spectrum of SN 2021aefx in the region around DNa I. We measure an equivalent width of W  λ  = 0.077 nm, corresponding to a host-galaxy extinction of E(B − V)host = 0.097 mag. Bottom: Milky Way extinction-corrected B − V color curve of SN 2021aefx. A linear fit to the color on the radioactively powered tail shows an offset of E(B − V)host = 0.044 mag with respect to the Lira Law. These are both consistent to within the scatter in the Lira Law, so we adopt the former estimate: E(B − V)host = 0.097 mag.