adsabs/AstroCLIMB huggingface dataset:
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Cumulative apparent peak magnitude distribution of KNe associated to O5 NS–NS (top row) and NS–BH (bottom row) GW events. The left-hand panels refer to the g band, while the right-hand ones are for the z band. Blue lines are for tightly localized events (Ω90% ≤ 20 deg2) while orange ones refer to events with 20 deg2 < Ω90% ≤ 100 deg2. The vertical dashed lines show our estimated 5σ single-visit depth for 30 and 180 s exposures, as annotated.
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Rubin observational cadences for NS–NS (top) and NS–BH (bottom) mergers follow-up with Rubin. Observations in the g + z filters will be replaced by observations in the g + i filters during bright dark time due to the limit of five filters available each night. For NS–NS mergers, we envision 30 s exposures in each filter on the first night, and 180 s exposures (markers circled in red) on the following nights. For NS–BH mergers, which are expected to be found at larger distances, 180 s exposures should be employed from the first night. Solid markers indicate planned observations over the entire localization area, while semitransparent markers indicate possible extra observations to be carried out if the optical counterpart has not yet been identified.
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Example of Rubin tiling of simulated GW skymaps for NS–NS mergers localized within Ω90% < 20 deg2 (left panel) and 20 deg2 < Ω90% ≤ 100 deg2 (right panel). The tiling pattern was created using gwemopt (Coughlin & Stubbs 2016) to include most (≳90%) of the integrated localization probability. We expect most skymaps with Ω90% < 20 deg2 to require four Rubin pointings or less to cover >90% of the probability area, accounting for small offsets to be applied between exposures to cover chip gaps.
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Cadences for BH–BH merger follow-up with Rubin. In dark time, observations in the g+i filters are preferred to r+i observations, to be carried out in bright time.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: STVs during our monitoring period. In each individual panel, there are two subpanels. The upper subpanel is for the light curve, while the lower subpanel is for the differential light curve of the two comparison stars plus a constant.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: The optical R-band light curve. The data from 1ES 2344 + 514 shown here were corrected for the host galaxy contribution and Galactic reddening.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: IDV on JD 2,457,367. The upper subpanel is for the light curve, while the lower subpanel is for the differential light curve of the two comparison stars plus a constant.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: The source of 1ES 2344 + 514 in the image from LSW.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: A demonstration of part of the data from 1997 October 10 to 13, including an ICME with start and end times indicated by the dashed vertical lines. From the top to the bottom, the first five panels represent the magnetic field B and its components Bx, By, and Bz; the solar wind velocity V; the thermal velocity Vth; the plasma parameters β; and the proton and α particle density obtained by moment analysis and nonlinear analysis, separately Np, Np,nl, and Nα,nl. The last panel shows the real label.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: An illustration of the proposed pipeline. {fi, i = 1,…,33} represents the feature vectors set, including 33 features, and x indicates the input. There are only 0 or 1 in the original output y* and final output y (“0” and “1” represent non-ICMEs and ICMEs, respectively).
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The overview of the proposed RU-net, where the purple arrow indicates the 1D convolution layer with kernel size 1 × 1 and sigmoid activation function, the red arrows denote the max pooling layer, the green arrows represent the upsampling module, and the yellow arrows indicate the residual module. The parts of the encoder and the decoder are presented in the light yellow and light green regions, respectively. The structure of the residual module is shown in the red dotted box, where xi indicates the input of the residual block, F( · ) and F(xi) represent the learned mapping and output of the convolution module separately, and H( · ) indicates the output of the residual block.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: A schematic diagram of the correction algorithm. From the top to the bottom are the ground truth, the raw predictions, and the processed predictions from 1997 November 22 to 24. The start and end times of the ICMEs are indicated by the dashed vertical lines. The difference and the overlap among the ground truth, the raw, and the processed predictions are denoted by the red box and the green box, respectively.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The detection results (P and R) of the different models. The blue zone and the yellow zone indicate the high precision region and the high recall region, respectively. The colored dots denote the time-series segmentation models, and the black line represents the precision–recall curve published in Nguyen et al. (2019).
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: Ablation study using the correction algorithm.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The time consumption of each module in the pipeline (Nguyen et al. 2019).
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The sum of the probabilities of each of the ICMEs in our test period as a function of the temporal shift to the closest predicted ICMEs. The blue dots and yellow dots indicate TPs and FNs, respectively, while the size represents the duration. The black line indicates the minimum among the TPs.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The predictions of a long TP (a), a short TP (c), and an FN (e), corresponding to the red dot in Figure 5, and their patterns on the magnetic field, as shown in (b), (d), and (f). The start and end times of these ICMEs are indicated by the dashed vertical lines.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: Histogram statistics of the duration (left) and sum of probability of the samples (right) during the period of TPs and FPs corresponding to RU-net (the red dot in Figure 5).
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The distributions of duration, magnet field, and thermal velocity of the predicted ICMEs and the test ICMEs.
Paper: RU-net: A Residual U-net for Automatic Interplanetary Coronal Mass Ejection Detection
Authors: Jun Chen, Hao Deng, Shuxin Li, Weifu Li, Hong Chen, Yanhong Chen, and Bingxian Luo
Figure caption: The performance of our pipeline using different data sets: the complete data set (the red nabla); only magnetic field information (the blue nabla); magnetic field, β, and proton flux information (the green nabla); and only proton flux information (the purple nabla). The black nabla represents the highest F1 score in Nguyen et al. (2019).
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Ecliptic longitude and latitude components of the observed relative velocity of the of the moving objects detected in the FOSSIL observations. The area outlined by red is used to select Hildas from the FOSSIL survey (see text for details). The FOSSIL Hildas with derived rotation periods are indicated in green, and those for which no period could be determined are indicated by red dots. The inset figure shows the ecliptic motions around the oppositions of known Hildas and MBAs around the area highly populated by Hildas (see main text). In total, 247 out of the 270 known objects in the Hilda selection area are Hildas, while the remaining 23 objects are high-eccentricity MBAs.
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Folded lightcurves of 12 Hildas where a double-peak fit was obtained. The object ID and derived rotation period are indicated on each plot. Different colors represent data points obtained from different nights. The gray lines are the fitted results. Photometric errors are too small to be seen in the plots.
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Five folded lightcurves of Hildas where a single-peak fit was obtained. The top plot in each frame shows the results from the original single-peak fits, and the bottom plots show the folded lightcurves when a double-peaked period was found in a second round of fitting. The object ID and half period are indicated on each plot. Symbols are the same as in Figure 2. Photometric errors are too small to be seen in the plots.
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Rotation period and spin rate vs. diameter for the FOSSIL Hildas (orange dots). Previously measured Hilda rotation periods obtained from the LCDB and Szabó et al. (2020) are shown using green and blue dots, respectively. The rotation periods of MBAs in the LCDB are shown in the background as gray dots. The green, orange, and gray dashed lines indicate rotation periods of 4, 3, and 2 hr, respectively.
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Spin rate vs. amplitude of FOSSIL Hildas (orange dots) and Hildas obtained from the LCDB (green dots) and Szabó (2020, blue dots). The background gray dots denote MBAs. The green, orange, purple, and gray dashed lines are the rotation-period limits for rubble-pile asteroids with bulk densities of 1, 1.5, 2, and 3 g cm−3, respectively, calculated from Equation (5).
Paper: FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids
Authors: Chan-Kao Chang, Ying-Tung Chen, Wesley C. Fraser, Matthew J. Lehner, Shiang-Yu Wang, Mike Alexandersen, Young-Jun Choi, A. Paula Granados Contreras, Takashi Ito, Youngmin JeongAhn, Jianghui Ji, J. J. Kavelaars, Myung-Jin Kim, Samantha M. Lawler, Jian Li, Zhong-Yi Lin, Patryk Sofia Lykawka, Hong-Kyu Moon, Surhud More, Marco Muñoz-Gutiérrez, Keiji Ohtsuki, Rosemary E. Pike, Tsuyoshi Terai, Seitaro Urakawa, Fumi Yoshida, Hui Zhang, Haibin Zhao, and Ji-Lin Zhou
Figure caption: Left: The periodogram of FOSSIL object FSAU02020328. The red circle indicates the best fit. The minima near the best fit are the aliases due to the 1 day observing cycle. The second set of minima on the right side is the half period. Right: The folded lightcurve of the same object. Different colors represent data points obtained from different nights.
Paper: Dwarf Irregular Galaxy Leo A. II. Suprime-Cam R and Hα Stellar Photometry
Authors: Rima Stonkutė, and Vladas Vansevičius
Figure caption: Color index differences of the 81 ST standards used for the R passband photometry calibration, (R − I) − (R − I)ST, vs. the calibrated (R − I) color index. The rms of color index differences is 0.027 mag.
Paper: Dwarf Irregular Galaxy Leo A. II. Suprime-Cam R and Hα Stellar Photometry
Authors: Rima Stonkutė, and Vladas Vansevičius
Figure caption: Photometry parameters for objects in the Leo A field; starlike and extended objects are indicated by black and red dots, respectively. Photometry quality parameters are plotted vs. R (22,944 starlike and 5280 extended objects) and vs. NA (21,036 and 4764, respectively) magnitudes in panels: (a), (b) the photometric errors, σ; (c), (d) the object-profile sharpness in respect to the PSF, sharpness; (e), (f) the accuracy of object-profile fitting with the PSF, χ2.
Paper: Dwarf Irregular Galaxy Leo A. II. Suprime-Cam R and Hα Stellar Photometry
Authors: Rima Stonkutė, and Vladas Vansevičius
Figure caption: The NA−R color index vs. R magnitude (a) and vs. B−V color index (b) of the bright (R < 23) starlike objects in the Leo A field plotted as gray dots. Two groups of stars with flux excesses (NA − R < −0.05) in the NA passband are overplotted: the Milky Way late-type stars (red dots) and the early-type emission-line stars (cyan dots). Dashed red and dashed blue lines show the regions occupied by the solar metallicity stars of spectral types later than K6V and earlier than A0V, respectively (Pecaut & Mamajek 2013). Blue dots mark objects with a significant flux excess in the NA passband that do not belong to the previous two groups of stars (red and cyan dots). Blue open circles mark stars with a significant flux deficit in the NA passband. Blue arrows mark objects beyond the limits of the figure; numbers adjacent to arrows indicate values of their NA−R color index.
Paper: Dwarf Irregular Galaxy Leo A. II. Suprime-Cam R and Hα Stellar Photometry
Authors: Rima Stonkutė, and Vladas Vansevičius
Figure caption: The R magnitude vs. R−I of 2008 bright starlike objects in the Leo A field. Symbols mark the same types of objects as in Figure 3. A blue arrow marks an object beyond the limits of the figure; a number adjacent to the arrow indicates the value of the R−I color index. The blue dashed line marks the main sequence (MS) and the red dashed line marks the red giant branch (RGB) of the Leo A galaxy.
Paper: Dwarf Irregular Galaxy Leo A. II. Suprime-Cam R and Hα Stellar Photometry
Authors: Rima Stonkutė, and Vladas Vansevičius
Figure caption: A spatial distribution of 2008 bright starlike objects in the Leo A field (R < 23 mag). Symbols mark the same types of objects as in Figure 3. The blue line ellipse indicates an approximate size of the Leo A galaxy—10′ along the major axis. North is up and east is to the left.
Paper: The First Data Release of CNIa0.02—A Complete Nearby (Redshift <0.02) Sample of Type Ia Supernova Light Curves  
Authors: Ping Chen, Subo Dong, C. S. Kochanek, K. Z. Stanek, R. S. Post, M. D. Stritzinger, J. L. Prieto, Alexei V. Filippenko, Juna A. Kollmeier, N. Elias-Rosa, Boaz Katz, Lina Tomasella, S. Bose, Chris Ashall, S. Benetti, D. Bersier, Joseph Brimacombe, Thomas G. Brink, P. Brown, David A. H. Buckley, Enrico Cappellaro, Grant W. Christie, Morgan Fraser, Mariusz Gromadzki, Thomas W.-S. Holoien, Shaoming Hu, Erkki Kankare, Robert Koff, P. Lundqvist, S. Mattila, P. A. Milne, Nidia Morrell, J. A. Muñoz, Robert Mutel, Tim Natusch, Joel Nicolas, A. Pastorello, Simon Prentice, Tyler Roth, B. J. Shappee, Geoffrey Stone, Todd A. Thompson, Steven Villanueva, and WeiKang Zheng
Figure caption: The cumulative redshift distribution of all SNe Ia (blue histogram) in DR1 and those in the complete sample (black histogram) from the CNIa0.02 project. The redshift limit of z = 0.02 for the complete sample is indicated with the dashed vertical blue line. An illustrative N ∝ z3 is plotted with the red line to indicate a simplified expectation from a volume-limited sample covering the full luminosity range by assuming a linear relation between distance and redshift. The distribution approximately follows the expectation for a volume-limited sample at z ≳ 0.01, for which peculiar velocities are negligible compared to the Hubble expansion velocity. The apparent excess of SNe with 0.005 ≲ z ≲ 0.013 with respect to the volume-limited expectation is probably contributed by the effects of peculiar velocities at low redshift and/or fluctuations due to small number statistics.