adsabs/AstroCLIMB huggingface dataset:
Paper: A Survey of Sulfur-bearing Molecular Lines toward the Dense Cores in 11 Massive Protoclusters
Authors: Mengyao Tang, Sheng-Li Qin, Tie Liu, Luis A. Zapata, Xunchuan Liu, Yaping Peng, Fengwei Xu, Chao Zhang, Ken'ichi Tatematsu
Figure caption: Violin plots for total abundance (upper panel) and the number of detected species (bottom panel). The regions with orange and blue colors represent the presence and absence of outflows, respectively. In each panel, the left plots are statistics of low-mass cores, and the right plots are statistics of high-mass cores. The dotted lines in the plots represent the quartiles.
Paper: A Survey of Sulfur-bearing Molecular Lines toward the Dense Cores in 11 Massive Protoclusters
Authors: Mengyao Tang, Sheng-Li Qin, Tie Liu, Luis A. Zapata, Xunchuan Liu, Yaping Peng, Fengwei Xu, Chao Zhang, Ken'ichi Tatematsu
Figure caption: The detection rate of S-bearing species. The upper, middle, and bottom panels present detection rates of all cores, prestellar core candidates, and protostellar cores, respectively.
Paper: A Survey of Sulfur-bearing Molecular Lines toward the Dense Cores in 11 Massive Protoclusters
Authors: Mengyao Tang, Sheng-Li Qin, Tie Liu, Luis A. Zapata, Xunchuan Liu, Yaping Peng, Fengwei Xu, Chao Zhang, Ken'ichi Tatematsu
Figure caption: The correlation between the nonthermal velocity dispersions (σ NT) of SO (upper panel) and SO2 (bottom panel) vs. their abundances. In each panel, high-mass cores and low-mass cores are shown as orange and blue colors, respectively. The Spearman correlation coefficient (r) is displayed in the upper-right corner of each panel.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: SESN discoveries since the first H-poor SN, SN 1954A (S. Pietra 1955). The top panel shows all SESNe, including SNe Ibc and peculiar subtypes (but excluding SLSNe), and the bottom panel shows only SNe for which >10 photometric data points have been published. The color band running at the top of the bottom panel represents the average number of photometric data points per SN, in log scale, and it runs from a minimum (purple) of 0 in years when no SNe were observed to a maximum (yellow) of 1838 data points in 1993, with the single best observed SESN: SN 1993J. The maximum number of discoveries with >10 photometric data points is reached in the 5 yr bin centered on 2004, but it is likely an artifact due to delayed publication: photometric observations often continue to appear in the literature in the decade following an object’s discovery.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Left: photometric coverage, in any band, for all 165 light curves in our sample, out to 100 days past peak. The names of SNe with more than 500 observations are explicitly indicated. As expected, most coverage is seen near peak, although a few light curves have consistently dense coverage throughout (e.g., SN 2007gr, SN 2011dh, SN 2006jc). Right: photometric coverage for all 165 light curves in our sample in each of the considered photometric bands: w2, m2, w1, U, u, B, g, V, r, R, i, I, J, H, K  s , as labeled. Uu, Rr, and Ii are plotted together. B, V, Rr, and Ii have the most coverage. The color bar reflects the mapping of color saturation to number for all subplots (illustratively shown in blue but consistent for all panels).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Redshift z distribution for all SESNe in the literature, as collected by the OSNC, and for the subsample we will use for template construction. Top: a histogram of the distributions in 10 bins. Bottom: box-and-whiskers plot of the distributions. A box-and-whiskers plot shows the median of the distribution as a vertical line, the 25th percentiles as a colored box (i.e., the IQR), and the bars, joined to each end of the box by a line, represent the minimum and maximum of the distribution excluding statistical outliers, where outliers are defined as any point farther than 1.5 × IQR from the edges for the IQR. The “outliers” thus defined are shown as data points. None of the SNe in the full literature sample exceeding z = 0.4 are in the selected “well-observed” sample that is used for template construction. At z = 0.4 the spectra are shifted by the typical width of an optical photometry band, so that the ﹩r^{\prime} ﹩ rest band, for example, would be observed in the ﹩i^{\prime} ﹩ filter. The template sample has a median of 0.017 and a 99.7th percentile (equivalent to 3σ in a Gaussian distribution) of 0.31. Notice that the low-z edge of the distribution is below zero: SN 1993J and SN 2004gk, extremely nearby objects, have negative recession velocities (z  = −1.13 × 10−4 and z = −5.50 × 10−4, respectively).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Top panel: the B-band median template for all SESNe generated as described in Section 4 is shown as a blue line along with the IQR (shaded region). Data points for all light curves used in the generation of the template are shown, labeled and colored by SESN subtype. Middle panel: same as the top panel, but for the weighted-average templates and their weighted standard deviation uncertainty region (IQR). Bottom panel: the median template (blue line) and the weighted-average template (purple line) are shown together to aid comparison, along with their respective uncertainties as shaded red and gray areas, respectively. The weighted-average template has larger uncertainties and is typically brighter owing to a photometric bias introduced by the use of the photometric uncertainty to weigh the data points. We ultimately select the rolling median procedure to generate SN Ibc templates. Note that the median template has a flatter top compared to the individual SESNe. This happens because we have forced the peaks to be at relative magnitudes of zero. However, the uncertainty region accounts for various SN shapes close to the peak.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Distribution of the S/N of the photometry used in this analysis. Different photometric bands are shown along the x-axis. For each band, the S/N distribution is shown as a violin plot where the distribution is smoothed via kernel density estimation and the median, IQR, and full extent of the distribution are shown by a white dot, thick gray bar, and thin gray line, respectively. While our photometric templates will be generated separately for each band, for the purpose of this plot the S/N measurements for ﹩u^{\prime} /U﹩, ﹩r^{\prime} /R﹩, and ﹩i^{\prime} /I﹩ are considered together. As expected, optical bands, and in particular V, B, and g, have a higher median S/N (19, 43, 29, 27, 38, and 36 for ﹩u^{\prime} /U﹩, V, B, g, ﹩r^{\prime} /R﹩, and ﹩i^{\prime} /I﹩, respectively) than NIR and UV bands (median S/N = 16, 11, 9, 8, 12 for H, K  s , w1, w2, m2, and median S/N of 26 for J) with the upper IQRs stretching out to S/N > 80 for optical photometry. Note that only uncertainties larger than 0.01 mag are used to calculate the S/N, generating an artificial cutoff in the distributions at high S/N.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Comparison of our templates with the templates published in D11. Our SN Ibc templates are plotted as a solid line in color, and the D11 templates are plotted as a solid blue line. D11's photometry suffers from galaxy contamination (see B14), but the templates are mostly based on well-sampled literature light curves, and therefore the contamination is likely not significant. The post-maximum light-curve decay is consistent with what we measure; however, the light-curve rise is far steeper for D11. Notice that the uncertainty on D11's templates, plotted in their Figures 2, 3, and 5, is not reproduced in our figure since it is not available online. Nonetheless, since this uncertainty simply represents the standard deviation of the sample and the early-time template behavior is based on one to a few light curves, the uncertainty as plotted in D11 goes to 0 in the earliest epochs and does not help reconcile the pre-maximum discrepancy between our template and the D11 templates. Nonetheless, the D11 templates match our Ibc templates very well after phase −15.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: The data-driven SN Ibc templates produced as a rolling median of all photometric data points available in each band as described in Section 4. The number of SNe used to construct each template is as follows: U: 39; u: 20; B: 75; V: 80; R: 41; r: 57; I: 27; i: 55; J: 23; H: 22; K  s : 18; w1: 15; w2: 15; m2: 9. The SN Ibc median template and its IQR are shown in each band as a solid line and shaded region, respectively. For reference, the V-band template is plotted in each panel (as a green dashed line).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Examples of SN light curves, from heterogeneous photometric sources. For each SN the date of V-band maximum ﹩{\mathrm{JD}}_{\max }﹩ is marked by a vertical black line, and its 1σ uncertainty is marked as a gray region (to enhance visibility, since the uncertainty is typically very small, the 1σ uncertainty region extends further above and below the ﹩{\mathrm{JD}}_{\max }﹩ line). SN 1993J V band (top) is very well sampled, possibly with underestimated uncertainties. SN 2002ap R band (middle) is well sampled around the peak, but it shows large gaps later. SN 2010bh I band is a sparsely sampled light curve with uncertainties conveying the scatter properly (bottom). Many publications are dedicated to each of these SNe: for SN 1993J the first articles appeared in 1993 (M. Okyudo et al. 1993), and the most recent at the time of writing is S. Zsiros et al. (2022). For SN 2002ap see A. Gal-Yam et al. (2002) and recent modeling work including E. Zapartas et al. 2017. For SN 2010bh see work including Y.-Z. Fan et al. (2011) and F. Bufano et al. (2012).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: From top left and moving clockwise: SN 1993J B band, SN 2004fe i band, SN 2009mg V band, and SN 2005kz r band. For each plot, the top left panel includes the time series, the SN Ibc template for that band, and the residual between the two, and the right panel shows the light curve along with its GP fit in the logarithmic time domain where the fit is performed. The bottom panel is the fit in natural time. The red line is the mean of the fit, and the gray band (occasionally too thin to see) represents the uncertainty (point-by-point standard deviation of the GP realizations). To learn more about SN 2009mg, see S. R. Oates et al. (2012).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: The SN Ibc templates made of all photometric data points available for all SESN subtypes (black curves) in each of the bands B, V, R, I. These templates are plotted, along with light curves of those SNe that have been claimed as prototypical of their class. For example, SN 1994I and SN 2005kl have been claimed to be prototypical SNe Ic, but they clearly deviate from our template.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Comparison of our templates with the templates published in T15 for the common bands ﹩u^{\prime} ,\,r^{\prime} ,\,i^{\prime} ﹩, accessed at the Vizier catalog J/A+A/574/A60/template on 2021 February 12. The rise portion of the templates, which was the focus of T15, is steeper than our rise, and the decay is slightly shallower in all bands. In ﹩u^{\prime} ﹩ and ﹩i^{\prime} ﹩, T15 templates seem to have weak signatures of shock breakout, but they seem to be dimmer than the lower range of the uncertainties of our templates.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Δm 15 (left) and Δm −10 (right) for our SN Ibc templates and each SESN subtype template. The location of the point on the x-axis is set to the effective wavelength of the filter (assuming the Swift UVOT system for w2, m2, w1; Johnson and SDSS filters for the U BV RI and ﹩u^{\prime} g^{\prime} r^{\prime} i^{\prime} ﹩, respectively; and 2MASS/PAIRITEL for J, H, K  s ). In the top panel, the values are separated on the vertical axis by an arbitrary value (as per the legend) for readability. In the bottom panel, the values are plotted in their natural space to make the overlap and separation of measurements more obvious to the eye. We see an overall slower evolution past peak as wavelengths get longer, both in the Ibc templates and in each individual subtype template. At the bluest wavelengths (w2, m2, w1) the photometric measurements are too sparse and too scarce to assess any wavelength-based dependence on the evolutionary timescales. In most photometric bands, the Δm 15 and Δm −10 are consistent for all subtypes within the uncertainties (IQR) except for the rapid post-peak evolution of SNe Ibn, discussed further in Section 5.8 (for which measurements of Δm 15 only are available in selected bands). Occasionally, we see inconsistencies between the values measured for the SN Ibc templates and for the individual subtype GP templates. For example, the SN Ibc templates show a more rapid evolution at NIR wavelengths than each subtype’s template. We attribute this inconsistency to the poor quality and sparsity of photometric measurements in NIR bands. Values plotted are reported in Tables 3 and 4. This figure is further discussed in Section 5.4.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Panels and colors as in Figure 11, GP fit to SNe IIb SN 2011fu, B. Our model captures well the small excesses at early times, which are a known characteristic of many SNe IIb (see, e.g., I. Arcavi 2017; M. C. Bersten et al. 2018; M. Orellana & M. C. Bersten 2022), associated with a shock-cooling component. However, the late fit shows high-confidence features on timescales of days that are likely unphysical (see phase ∼60 days). To learn more about SN 2011fu, see B. Kumar et al. (2013) and A. Morales-Garoffolo et al. (2015).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: GP templates are shown in optical bands of ﹩U,\,u^{\prime} ,\,B,\,V,\,g^{\prime} ,\,R,\,r^{\prime} ,\,I,\,i^{\prime} ﹩ for each SESN subtype (as per the legend at the top). Templates of different subtypes in each band are behaving mostly similarly within the uncertainties. The behavior of the templates in different bands is consistent with our expectation of the decline becoming shallower as we move to redder bands. Sudden changes in the number of light curves used to generate the templates at some epochs may lead to unphysical behaviors such as the rapid increase in the uncertainty of the Ib U-band template near ∼30 days or the uncertainty drop in the Ic g-band template between ∼35 and ∼50 days from ﹩{\mathrm{JD}}_{{\rm{}}\mathrm{Vmax}}﹩.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: GP templates of subtypes Ic and Ic-bl in all the existing bands. The lower plot in each panel shows the number of light curves that were used in each time window to create the template. We caution the reader that sharp features in the templates or their uncertainties can be connected to the sudden change in the number of light curves used to generate the template in that band (e.g., Ic template near 40 days after ﹩{\mathrm{JD}}_{V\max }﹩).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for SN IIb and SN Ic-bl subtypes.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for SN Ib and SN Ic-bl subtypes.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: SN 1993J U: color and panels are as in Figure 11. The small uncertainty in the data causes an overfit with any choice of parameters that leads to the late-time bump at ∼30 (which is most apparent in the log fit top panel). Inflating the error bars by a factor ∼10 gives a more realistic fit at late times, at the cost of losing details at early times (including the cooling-envelope-related early excess).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: GP templates for the w1, J, H, and K  s  bands. There are less than three light curves in the w2 and m2 bands, and we are not able to release a template for these bands.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: SN 2010al V: color and panels are as in Figure 11. The light-curve sampling ends before 60 days, and the GP fit shows an upturn toward the end, which is an artifact of the fit and not a feature of the SN photometry.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: The GP templates of subtypes Ib (blue curve) and Ibn (purple curve) are plotted, along with ELAsTiCC light curves of SNe Ib in u, g, r, i bands (black dots) and their per-day medians (pink diamonds). The ELAsTiCC sample is broadly consistent with the SN Ib behavior observed in our sample, although they display a larger variance. Some of the light curves in the ELAsTiCC sample have a rapid evolution broadly consistent with SNe Ibn.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: The GP template of subtype Ic (green curve) is plotted, along with ELAsTiCC light curves of SNe Ic in u, g, r, i bands (black dots) and their per-day medians (pink diamonds). The ELAsTiCC sample shows a significantly more rapid rise for SNe Ic than observed in our sample in the r and i bands. The fall is broadly consistent with the past-peak behavior of our sample, but, as for Figure 22, the ELAsTiCC sample shows a larger variance than observed in our data.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 25, but for SNe Ic.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: The GP template of subtype Ic-bl (orange curve) is plotted, along with ELAsTiCC light curves of SNe Ic-bl in g, r, i bands (black dots; no data are available in u band) and their per-day medians (pink diamonds). The ELAsTiCC data show a behavior broadly consistent with our SN Ic-bl sample. We note a deviation in late-time behavior in r band (phase >20 days), but our templates are rather noisy in this region.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: GP templates for the SN IIb subtype are shown in bands B, V, I (black curves), along with their IQR (gray shaded area). In each band, light curves of SNe with unusual spectroscopic or photometric features are plotted to compare their photometry with the GP templates.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 25, but for SNe Ib.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Our GP templates (solid lines) are plotted, along with the most well-sampled PLAsTiCC light curves of SNe Ibc in u, g, r, i bands (gray dots). Compared to our templates, the PLAsTiCC simulations show significant differences: they have light curves with slower late-time evolution, particularly in the redder bands, as well as a few extremely fast evolving light curves.