adsabs/AstroCLIMB huggingface dataset:
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The synthetic spectra generated by the spectrum synthesis method on the KPNO-NIR solar spectrum for the selected neutral and ionized iron lines. The computed profiles illustrate the synthetic spectra for the three varying logarithmic abundances. The red lines are the spectra computed with no contribution from those neutral and ionized iron lines.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The KPNO-NIR solar spectrum and the number of identified lines in the respective wavelength regions (each bar indicates 50 Å region of the spectrum).
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The positions of HD 76151 on the Kiel and color–magnitude diagrams. The blue curves show the PARSEC isochrone representing the star, and the magenta dashed curves represent the uncertainties taken into account in the age determination.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: There are three physical aspects that control the boil-off and core-powered mass-loss processes. First, the H/He mass that maintains the RCB density and replenishes the outflow must be lifted from the deep part of the envelope; this is known as the envelope re-equilibration (orange). In GSS16, this was argued to be the bottleneck due to the limited amount of intrinsic cooling energy L int available to overcome the gravitational force, resulting in an energy-limited escape. Second, the outflow in the radiative zone is fueled by the stellar bolometric luminosity and by L int (blue). We propose that when L int is insufficient to drive the full outflow, another bottleneck exists in the deep atmosphere below a critical optical depth τ  h , where the absorption of the bolometric energy a planet receives is inefficient, shown in red. Third, an efficient core luminosity keeps the H/He envelope warm and large in radius, which consequently elevates density at the sonic point, encouraging a more substantial mass loss.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: The top panel shows the relevant timescales for energy and radiation re-equilibration in the convective envelope: turnover timescale of the mixing (solid), eddy diffusion timescale (dotted), and dynamical timescale (dashed). The physical processes that mix and propagate energy and material are faster than the shortest mass-loss timescale ∼1 yr at the beginning of boil-off, validating our isentropic and adiabatic assumption for the envelope (see Section 3.1.1). The middle panel shows the convective mass flux vs. the mass-loss rate of non-energy-limited isothermal Parker wind boil-off, implying that the advective wind cannot penetrate deep into the envelope, as the envelope is convection dominated. In the bottom panel, the internal energy transport through E conv is sufficient to lift H/He material out of the envelope. This is for a 3.6 M ⊕ planet irradiated with 100 F ⊕. The same model planet is used for Figures 3–7.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: With our numerical model, we show the evolution of the H/He mass fraction (top) and mass-loss rate (bottom) under different types of mass loss: non-energy-limited isothermal Parker wind (black), mass loss limited by the total bolometric luminosity available (light gray), and mass loss limited by the “bottleneck” region below τ  h  (dark gray), where the energy is assumed to be taken from the intrinsic luminosity. These decoupled Parker winds are compared to the GSS18 energy-limited prescription (red). The first and second types of the decoupled Parker winds, namely “bolometric-limited” and “intrinsic-limited mass” loss, start to be not energy limited before the boil-off ends. The transition time is indicated with circles. Consequently, the final mass fractions from all of these decoupled Parker winds converge to a common evolution track by the end of the boil-off at ∼1 Myr, proving that our default non-energy-limited isothermal Parker wind assumption does not affect the long-term evolution. The vertical dashed line shows the transition time when boil-off ends. The original GSS18 model shows a continued mass loss at old ages.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show an example of the evolution of a 3.6 M ⊕ planet irradiated with 10 F ⊕ flux based on our numerical model. The three black-and-white panels show the planetary radius, core temperature, and mass fraction of H/He, while the color panel shows the interior and atmosphere P−T profile from 1000 yr to 10 Gyr. The RCB and the core−envelope boundary (CEB) are marked by crosses and circles, respectively. Below the RCB is the convective H/He envelope, which is adiabatic, and the rock/iron core, assumed to be isothermal, constitutes the deepest part of the interior below 104 bar. Based on the relative timescales between mass loss and thermal evolution, we define the boil-off phase and long-lived post-boil-off phase shown with dashed and solid lines, respectively. The elements of the model are more fully described in Section 3.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the change of total energy (gravitational binding energy and thermal energy) as a result of mass loss alone (excluding thermal contraction and mass transfer to the radiative atmosphere; see Equations (20) and (26)) in between two consecutive static structure models, in solid black. This is compared (in solid gray) to the analytically derived energy that is needed to power the wind being lifted from the surface of the convective envelope. Our results demonstrate that the escaping material can be treated as being taken from the surface of the convective envelope (the RCB) rather than the deep interior, as the mass transport within the adiabatic envelope is powered by the internal energy of the envelope (see Section 3.1.2). As for the deep radiative layer (above τ  h ), the energy needed (dashed black line) can be approximated by a steady-state isothermal wind (dashed gray line) given enough energy supply to power the wind (see Equations (19) and (25)). As a comparison, the energy needed from the original GSS16 work is shown in dashed red. Notably, the bottleneck (dashed) suggested in our work is less severe.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the ratio between the energy needed to overcome the PdV work and the direct stellar bolometric absorption as a function of the optical depth to visible photons τ  ν , calculated based on Equation (23). Given that the whole radiative atmosphere can get a sufficient amount of the bolometric energy, the bottleneck happens below τ  h  ≈ 10 (dashed line), as the bolometric flux becomes too tenuous to efficiently sustain the energy need to lift the H/He material. In this case, another energy source, e.g., intrinsic luminosity, is needed in order to further transport material from the RCB (circle) to the radius where τ  ν  = τ  h .
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the energy sources (black lines) available to power the hydrodynamic wind: intrinsic cooling energy from the interior radiation (black solid line) and stellar bolometric energy (black dashed line). In the red lines, we show the energy required to overcome PdV work in order to lose mass, for both the entire radiative region (red dashed line) and the bottleneck layer below the τ  h  surface (red solid line). The stellar bolometric radiation limits the efficiency of mass loss before 1 kyr, denoted as bolometric-limited escape. However, the energy barrier that restricts the wind outflow continues until 10 kyr owing to the inadequacy of intrinsic luminosity supply in the bottleneck region, which we call intrinsic-limited escape.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The μ PDF behavior of the 202 MW-analogous host–satellite systems in TNG50-1 as a function of the two parameters: min(α  N ) and 〈d〉norm. The x-axis represents the parameterization of the radial concentration of satellites (〈d〉norm), where smaller values indicate a more center-concentrated system. The y-axis represents the parameter for orbital pole alignment (min(α 8)), with smaller opening angles indicating better-aligned orbital poles (higher kinematic coherence). We break down the parameters into 15 smaller intervals. For each min(α  N ) vs. 〈d〉norm grid, we generate μ PDF of SKASs for 103 random host–satellite systems and take their median value. The white-to-black color bar on the right-hand side illustrates the median of 103 μ PDF. Left-hand panel: the contours (dotted lines) show the iso-c/a loci with the 1σ uncertainty bands. Note that a more aligned set of orbital poles and a more centrally concentrated satellite distribution contribute to a flatter structure. Right-hand panel: the same as the left-hand panel but shows our data without uncertainty bands for clarity. The locations of the TNG50-1 systems (small blue dots and a large blue circle with an error bar), the MW (black large star), and the full-randomized system (black large circle) are denoted. It is evident that both parameters of the MW DoS significantly favor a planar configuration compared to those of the TNG50-1 host–satellite systems.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The difference between the median of the c/a PDF and present-day c/a for the 105 SKASs of 202 MW-analogous host–satellite systems in TNG50-1. Left-hand panel: for the examples of 16 randomly selected systems, we show the intrinsic c/a PDFs (blue histograms), their median values (vertical solid blue lines), and the measured c/a values (vertical dotted black lines). The difference between the median of the c/a PDF and measured c/a are marked as gray rectangles. Right-hand panel: we show the distribution of the differences between the median of the c/a PDF and measured c/a for the total 202 MW-analogous host–satellite systems. The vertical solid black line at 0.025 indicates the median of the differences.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: Left-hand panel: the relation between μ PDF and present-day c/a of the MW (black star) and the 202 MW-analogous host–satellite systems in TNG50-1 (blue dots). The dashed black line denotes the one-to-one relation. Although present-day c/a roughly follows μ PDF, the spread is sizeable. Right-hand panel: the relation between the rarity based on μ PDF (x-axis) and the rarity based on present-day c/a (y-axis) for the MW (black star) and the 202 MW-analogous host–satellite systems in TNG50-1 (blue dots). The dashed black line denotes the one-to-one relation. We note that there is no correlation between the two types of rarity. The MW (black star) is located at the bottom left-hand corner of the plot, indicating that it comes out rare in both criteria. However, the rarity based on c/a should be taken as a by-chance occasion.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The c/a PDFs (left-hand panel) and their corresponding μ PDF (right-hand panel) for the MW and 202 MW-analogous host–satellite systems of the TNG50-1 simulation. Left-hand panel: we show the intrinsic c/a PDFs of 202 systems in TNG50-1 (thin blue loci) and the MW DoS (thick black locus). All c/a PDFs are quite broad. The vertical solid black line is for μ PDF of the MW DoS at 0.347. Right-hand panel: we show the μ PDF distribution of all 202 systems. The vertical blue dotted line is for the median of μ PDF of 202 systems at 0.462. The solid black line is for μ PDF of the MW DoS at 0.347. The rarity of the MW DoS based on μ PDF is calculated to be 2.48% (=5/202).
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The c/a PDF of 105 SKASs for the MW DoS. The x-axis is for c/a and the y-axis is for the number of SKASs within the corresponding c/a bins. The c/a PDF of the MW DoS is quite broad (σ  c/a  ∼ 0.105), implying that a simple present-day c/a value, combined with its highly time-variable nature, cannot fully represent the degree of flatness. The vertical solid black line indicates the median of the c/a PDFs at 0.347. The vertical dotted black line represents the observed present-day c/a of the MW DoS at 0.181, which is ∼1.8σ way from the median of the c/a PDFs.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The process of constructing our SDG and generating the SKASs. Left-hand panel: the orbital pole directions of satellites ( L ) are initially set based on a simulated host–satellite system of interest. Middle panel: The distances from the host galaxy to the satellites ( D ) are assigned based on the reference simulated system, forming circles along which satellites can be positioned. Right-hand panel: the orbital phase angles (ϕ) of satellites are given randomly on the circles, completing a system that meets the definition of the SKAS for the reference system.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: Aitoff projection plot of the orbital poles of 11 classical satellites of the MW. Each circle represents the galactic latitude (b) and longitude (l) of a satellite’s orbital pole. Hollow circles indicate the orbital poles from S. Shao et al. (2019), while filled circles represent the orbital poles used in this study, sourced from M. S. Pawlowski & P. Kroupa (2020), S. Taibi et al. (2024), and P. Bennet et al. (2024). We note that min(α 8) increases from 22° to 31.°6 due to the updated velocity data affecting the orbital poles of Leo I and Leo II.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The c/a distributions of 202 MW-analogous host–satellite systems in the TNG50-1 simulation. The x-axis represents present-day c/a and the y-axis indicates the number of systems within each c/a bin. The vertical solid blue line indicates the median c/a of the total 202 systems, and the vertical dotted black line corresponds to the observed c/a of the MW DoS. The degree of rarity of the MW DoS is 1.49%.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as Figure 1, but for two other satellite selection methods. Each panel shows the present-day c/a distribution for our fiducial selection method (left-hand panel), all SUBFIND selection method (middle panel), and the distance-limited selection method (right-hand panel).
Paper: A Catalog of Pulsar X-Ray Filaments
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: Stacked, exposure-corrected CXO observations of known (top) and candidate (bottom) filaments. Regions used for spectral fitting for filaments, antifilaments, and trails are marked with dotted lines. Bright point sources have been removed. The pulsar position is marked with a star and the proper motion indicated if known or assumed. Celestial north points up.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Example of LC fits for SN 2020tkx. Top panel: the photometry in flux space together with the GP interpolation and fit to the Bazin formula. This allows for estimates of peak time and other LC parameters, provided in Table 3. Peak magnitudes are shown in r band, along with the derived explosion epoch. Second panel: the absolute magnitude LC, along with the GP inteprolation and best-fit Bazin function. SN 1998bw’s LCs are plotted as comparison. The blue arrows indicate epochs when spectra were taken. Third panel: the color evolution, along with that of SN 1998bw. The template shown is a range of colors for normal stripped-envelope SNe from J. Sollerman et al. (2022). Bottom panel: the bolometric luminosity LC, along with the best-fit W. D. Arnett (1982) model.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Investigation of the Malmquist bias on the sample. ﹩{{M}}_{{\rm{r}}}^{\max }﹩ and the distance modulus (μ) for the events are plotted, with the minimum absolute magnitude (−16.86 mag) of the sample shown as a black dashed horizontal line. The distance modulus where the sample is complete (μ = 35.86 mag) is shown as a black dashed vertical line. One magnitude by one magnitude bins are marked by dashed blue lines, where the cutoff distance for the sample is marked by a black dashed vertical line. The random simulated events created through the method described in D. Richardson et al. (2014) are shown as red circles. The overall effect of the Malmquist bias is a 0.2 mag decrease in the overall average ﹩{{M}}_{{\rm{r}}}^{\max }﹩ of the sample.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Light-curve and color comparison bewteen the SNe Ic-BL sample and SN 1998bw in r/R- and g/B-bands, with all magnitudes corrected for Galactic extinction, and the GP-processed LCs shown. The colors are computed with a combination of the data binned within 1 day, as well as the GP-processed LCs. The LC of SN 1998bw (A. Clocchiatti et al. 2011) was interpolated through GP techniques, and is shown as the black dashed lines.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Comparison of V  ϕ  perturbations obtained by subtracting azimuthal average background (left) and Keplerian background (right) from the original FARGO3D simulation results. Note that the color bars are in linear scale and the ranges differ between these two groups of panels.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:                       ﹩{{M}}_{{\rm{r}}}^{\max }﹩ distribution of the SNe Type Ic-BL sample, with the mean magnitude (−18.51 mag) shown with a solid line and the standard deviation (0.90 mag) range shown with dashed lines.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Redshift distribution for the SNe Ic-BL sample.