adsabs/AstroCLIMB huggingface dataset:
Paper: H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4 
Authors: Yan Tan, Frances M. Skinner, Shanelle Samuels, Robert J. Hargreaves, Robab Hashemi, Iouli E. Gordon
Figure caption: The calculated opacity for NH3 transitions in the ν 2 band broadened by self, H2, He, H2O, and CO2 at a pressure of 1 atm and temperature of 296 K. Example includes a mixture where only H2 and He present at relative concentrations commonly assumed to be in gas giants. Note that the vertical scale on this plot is logarithmic on the bottom panel and linear on the top panel to show the effect both in core and wings of the lines. A sample of the code used to calculate these cross sections is given in Listing 1.
Paper: H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4 
Authors: Yan Tan, Frances M. Skinner, Shanelle Samuels, Robert J. Hargreaves, Robab Hashemi, Iouli E. Gordon
Figure caption: The H2 broadening of PH3 as a function of ∣m  J ∣ and K. The resultant ﹩{\gamma }_{{{\rm{H}}}_{2}}﹩ values (shown as the shaded surface) were obtained from a fit to the measured values of Sergent-Rozey et al. (1988), Butler et al. (2006), Bouanich et al. (2004) and are indicated by the color bar for clarity. The fitted coefficients for Equation (6) are provided on the left of the plot.
Paper: H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4 
Authors: Yan Tan, Frances M. Skinner, Shanelle Samuels, Robert J. Hargreaves, Robab Hashemi, Iouli E. Gordon
Figure caption: The CO2-broadening coefficients (﹩{\gamma }_{{\mathrm{CO}}_{2}}﹩) for H2CO have been estimated from their corresponding air-broadening (γ air) values. The ratio between the measured CO2 broadening by Wang & Sharples (2012) vs. HITRAN air-broadening values gave an average value of 1.848. This factor was used to scale the air-broadening data (shown in blue), resulting in the final CO2-broadening data for H2CO (given in black) to retain the rotational dependence.
Paper: H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4 
Authors: Yan Tan, Frances M. Skinner, Shanelle Samuels, Robert J. Hargreaves, Robab Hashemi, Iouli E. Gordon
Figure caption: The H2-broadening half-widths (﹩{\gamma }_{{{\rm{H}}}_{2}}﹩) for H2S as a function of index, J + 0.2K  a . The Padé approximant is plotted as the red line on the upper panel using Equation (3), and the blue line is a cubic polynomial function using Equation (1), showing advantage of the Padé approach. The experimental data sets with error bars were taken from Kissel et al. (2002), and the lower panel indicates the standard deviation determined from the fitting residuals is around 7% for ∣m∣ < 12.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The long-term lightcurve of 3C 454.3, where the black dots stand for the data collected from the literature and the red dots stand for the observations from this work.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The g, r, and i fitting results of the seven comparison stars. The black solid dots stand for U, B, V, R, and I data, the red solid dots stand for g, r, and i data, and the red lines stand for the least-squares fitting curves.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The quasi-period calculated by the Jurkevich method. The black line stands for the Jurkevich result and the red line stands for the smoothing curve.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The g, r, and i lightcurves. The black solid dots stand for the g lightcurve, the red solid dots stand for the r lightcurve, and the green solid dots stand for the i lightcurve.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The intraday optical variabilities at the g band.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The intraday optical variabilities at the i band.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The intraday optical variabilities at the r band.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: Comparisons of the predicted multiwavelength spectra of 3C 454.3 using the observations from this work (red dots) and NED (black dots). The red, green, blue, olive, violet, dark yellow, and navy dotted–dashed lines stand for the synchrotron, SSC, thermal (DISK), thermal (DT), EC (DISK), EC (BLR) and EC (DT) spectra respectively. The cyan line stands for the combination of the upper total spectra.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The comparisons between intraday variable timescales (ΔT) and variable values (Δm) at different bands. The black, red, and green lines stand for the results from the g band, r band, and i band respectively.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The distributions of ΔT. The left panel stands for the ΔT distributions and Gaussian fitting, and the right panel stands for the distributions of the correlation coefficient (r) from different order Gaussian functions.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The fitting curve for the long-term lightcurve based on a sine function. The black dots stand for the lightcurves and the blue dash curve stand for the fitting curve.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The quasi-period calculated by the power spectrum. The black line stands for the signal and the colorful dot lines stand for the theoretical red-noise spectra of 70%, 80%, 90%, 95%, and 99% significance level respectively.
Paper: Optical Monitoring and Variability Analyses of the FSRQ 3C 454.3
Authors: Y. H. Yuan, G. G. Wang, H. B. Xiao, J. H. Fan, H. R. Huang, G. Z. Ding, G. Z. Wen, F. J. Wu
Figure caption: The quasi-period calculated by the weighted wavelet Z-transform (WWZ), where, the left panel stands for the two-dimensional contour map of WWZ, and the right panel stands for the time-averaged WWZ power.
Paper: GST Data-processing Workflow: Image Registration and Alignment
Authors: Xu Yang, Wenda Cao, Vasyl Yurchyshyn
Figure caption: GST/BFI TiO to SDO/HMI I  c  image registration for AR NOAA 12371 with the SIFT method. Panels (a) and (b) illustrate the SIFT feature extraction process for the BFI/TiO image and HMI/I  c  image. Panels (a1) and (b1) are the original BFI/TiO and HMI/I  c  images displayed in their corresponding camera coordinates. In (a2) and (b2), the extreme dark/bright solar features are blocked out by an image mask from its median intensity. The colored circles in (a3) and (b3) are generated by the SIFT method. The green circles in panel (c) present first-matching points generated by FLANN. Blue lines and red lines distinguish the correct matches and fault matches, respectively, determined by RANSAC. Panel (d) is a BFI/TiO and HMI/I  c  combined image resulting from a successful registration, and it is plotted in a heliocentric coordinates map. The background is the HMI/I  c  and the registered TiO image is filled inside the black rectangle. The GST FOV has been cropped to better present the reference-checking points.
Paper: GST Data-processing Workflow: Image Registration and Alignment
Authors: Xu Yang, Wenda Cao, Vasyl Yurchyshyn
Figure caption: GST data registration and alignment workflow chart.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Comparison of the spectra of DIB λ10780 (this study) and K I 7699 Å for six targets, which were used to determine the rest-frame wavelength of DIB λ10780. The spectra of the K I absorption lines were reproduced from Welty & Hobbs (2001; for HD41117, HD141637, HD144470, and HD154368) and Siebenmorgen et al. (2020; for HD170740 and HD147889). The integration ranges of the DIB absorption are shown by the yellow areas. The central velocities measured from the profile of DIB 10780 are marked with the vertical black lines. The K I velocities weighted with the column densities of each velocity component are shown by the gray dashed lines.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Variations of the telluric lines with the observation sites and seasons. The normalized WINERED spectra of the telluric-standard stars obtained using the NTT in June (top), the Araki telescope in December (middle), and the Araki telescope in August (bottom) are shown.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Comparison between the velocities determined by DIB λ10780 (λ rest = 10780.6 Å) and those with a K I line (left) and the ﹩{{\rm{C}}}_{60}^{+}﹩ DIB λ9577 (right). The stars with FWHM 10780 < 1.5  Å are shown with red diamonds, and those with FWHM 10780 < 1.5  Å are shown with black circles.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption:  E(B–V) distribution and the spectral types of our targets.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Summary of the mesospheric CO lines we observed in each spectrum. The lines are shifted in velocity to the laboratory frame and in intensity to the zenith. The lines are sorted vertically by scan number and horizontally by observing season. The dates on the left are only approximate because owing to weather and other delays, scan numbers did not increase linearly with time. The year noted at the top corresponds to the start of the observing season, which typically runs into May of the following year. Horizontal gaps in the stacked lines are due to ranges of scan numbers that were eliminated during the data processing and were subsequently repeated.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Collection of the spectra over our entire sample and their corresponding synthetic model calculated using XCLASS. The black solid line shows the observed spectra and the orange solid line shows the fit obtained using the XCLASS software. In the lower panels of each graph, we plot the dispersion of the residuals (e = I obs − I model).
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Typical frequency-switched spectrum from the survey, taken at an elevation of 70°.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Histogram of the final rms noise in each of the 382,202 spectra in the survey.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Integrated maps for the high-intensity iCOM lines on the different transitions.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour maps of the blue- and redshifted emission of MF at (a) G351.77-0.54 and (b) G351.45+0.66. The respective central frequency and physical scale are labeled. The contour maps show the emission up from 66% + 10% peak emission; the blue and red contours stand for the blue- and redshifted emissions, respectively. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP for each emission line.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Dispersion of the integrated emission of CH3OH at 216.945559 GHz vs. the shock tracer SiO. The lower-right label shows the values for a linear fit in the log–log space. The upper outlier is the most chemically active source in our sample G327.29-0.58. This correlation points out that the shock environment in massive protostars favors the CH3OH gas-phase population.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour maps of the blue- and redshifted emission of methanol at (a) G328.81+0.63 and (b) G340.97-1.02. The respective central frequency and physical scale are labeled. The contour maps show the emission up from 66% + 10% peak emission; the blue and red contours stand for the blue- and redshifted emissions, respectively. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP for each emission line.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour maps of the blue- and redshifted emission of methanol at (a) G351.77-0.54 and (b) G351.45+0.66. The central frequency and physical scale are labeled. The contours show the emission up from 66% + 10% peak emission; the blue and red contours stand for the blue- and redshifted emissions, respectively. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP in the emission line.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour maps of the blue- and redshifted emission for several iCOMs detected in G327.29-0.58. The corresponding species and its central frequency is labeled in each frame. The contour maps show the emission up from 66% + 10% peak emission; the blue and red contours stand for the blue- and redshifted emissions, respectively. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP for each emission line.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour maps of the blue- and redshifted emission of MF at G333.13-0.43. The central frequency and physical scale are labeled. The contours show the emission up from 66% + 10% peak emission; the blue and red contours stand for the blue- and redshifted emissions, respectively. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP for each emission line.
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: G327.29-0.58 observed spectra averaged inward to the central 10″ from our central position (black solid line) and their corresponding synthetic modeling using XCLASS software (orange solid line). We also labeled the main contributing species to the spectra. In the lower panel, we displayed the residuals (e = I obs − I model).
Paper: Interstellar Complex Organic Molecules in SiO-traced Massive Outflows
Authors: O. S. Rojas-García, A. I. Gómez-Ruiz, A. Palau, M. T. Orozco-Aguilera, M. Chavez Dagostino, S. E. Kurtz
Figure caption: Contour map of the blue- and redshifted emission of the blended line conformed mainly by ethyl cyanide and acetone at 217.191 GHz toward the G327.29-0.58 region. The emission is tracing the core region. The contours show the emission up from 66% + 10% peak emission. The shifted emissions were integrated outward from the central 8 km−1 to reach the FWZP for each emission line.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Velocity-integrated CO intensity over the entire northern sky. It was derived by integrating the combined moment-masked cube (No. 5 in Table 3) over velocity from −36 to 36 km s−1, the full range over which significant emission is detected. For cosmetic purposes, the map was interpolated to 1/8° spacing and smoothed slightly by convolution with a 0.°3 Gaussian. The white area is unobserved.(The data used to create this figure are available).
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Average of all the mesospheric CO lines observed during the 2001–2002 season with the fit of a Gaussian plus Lorentzian function overlaid. As in Figure 3, the lines have been shifted in velocity to the laboratory frame and in intensity to the zenith. The Gaussian peak amplitude and dispersion are 0.167 ± 0.011 K and 0.410 ± 0.006 km s−1, and the Lorentzian peak amplitude and width parameter are 0.185 ± 0.012 K and 0.622 ± 0.025 km s−1. Both functions were assumed to be centered at 0 km s−1.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Integrated intensity of the mesospheric CO line at the zenith averaged in 1 hr bins during a five-day period in 2002 February. The error bars are 1σ based on the instrumental noise.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: A finder chart for most of the molecular clouds we have identified in the northern sky at ∣b∣ > 20° (Table 2). The colors here simply help to distinguish individual clouds. For clarity, we have zoomed in on the crowded regions of Figure 8. The small number of clouds outside the limits of this chart can be readily identified from Figure 8 and Table 2.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Map of the peak LSR velocity for all nonzero positions in Figure 8. It was derived from the combined moment-masked cube (No. 5 in Table 3). At ∣b∣ > 20°, the peak velocities should correspond closely to the mean cloud velocities given in Table 2. Near the Galactic plane, however, the emission is complex and the velocities extend beyond the range represented by the colors.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Latitude–velocity map of CO emission integrated over the full longitude range of the present survey (No. 5 in Table 3). Outlier clouds are identified by their numbers in Table 2.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Demonstration of the ability of moment masking to reveal weak emission in a large survey. Average of all 382,202 of the new high-latitude CO spectra before (a) and after (b) moment masking was applied to the survey. Note that the emission evident in (b) is on an intensity scale that is 10 times lower than that in (a).
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Mesospheric CO line profiles for the 2010–11 observing season, as in Figure 3, before (a) and after (b) the mesospheric line removal described in Section 3.
Paper: A CO Survey of the Entire Northern Sky
Authors: T. M. Dame, P. Thaddeus
Figure caption: Histogram of the mean cloud velocities given in Table 2.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Upper panel: overview of DIBs from the optical wavelength range to the K band. The circles show the DIBs of HD183143. The circles show the DIBs detected or confirmed in H15 (blue), and the DIBs detected in this study (red). The black squares show the DIBs detected in the literature (Joblin et al. 1990; Foing & Ehrenfreund 1994; Groh et al. 2007). The green diamonds show the DIBs detected in Ebenbichler et al. (2022). The gray and black circles show the DIBs in the range of 4000–9000  Å (Fan et al. 2019) and the H-band DIBs (Cox et al. 2014), respectively. For the DIBs in the K band and some weak DIBs in the H band, we adopt the DIB EWs for Cyg OB2 No. 5 from Galazutdinov et al. (2017b), because, to date, these DIBs have not been detected toward HD183143. Note that the points of No. 5 are only plotted to show the DIB distribution at the longest wavelength, and cannot be directly compared with the other data from HD183143, owing to the difference in the DIB EWs between HD183143 and No. 5. The gray shaded areas show the wavelength ranges in which we could not search for DIBs, owing to strong telluric absorption. Lower panel: synthetic spectrum of telluric absorption created by ATRAN (Lord 1992).