adsabs/AstroCLIMB huggingface dataset:
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Top panel: distribution of RGB stars used in this work on the Teff−log g plane colored by age. Middle panel: the density distribution of RGB stars in the R, Z plane and the number of stars in the north of the Galactic disk (122402) is more than that in the South (91985), which is normalized by the total number. Bottom panel: distribution of RGB stars in the Galactic longitude and latitude coordinate system. Younger stars are nearer the low-Galactic latitude naturally, in the meanwhile older stars are mainly distributed in the high-Galactic latitude.
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: The velocity (v) and the velocity dispersion (σ) maps of stellar, balmer, and forbidden lines for the NGC 3182. The solid circles indicate the inner and outer boundaries of the star-forming ring. The inner and outer dashed circles imply the S/Ncontinuum of ∼30 and 20, respectively. Hα> 1.5 Å. [N II] or [O III] > 1.5 Å.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Similar to Figure 12 but for young OB type stars. Normalized density in the vertical velocity and angular momentum plane. Top one is the entire sample, middle one is sample distribution in the north side, and bottom one is sample in the south side. Three panels are showing the break discovered in the recent works, which is far clearer and stronger than RGB sample.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Normalized density in the vertical velocity and angular momentum plane. The top part is the entire sample, the middle part is sample distribution in the north side, and bottom one is sample in the south side. Two arrows in the three panels are showing the break discovered in the recent works, especially for the middle one.
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: Hβ vs. [MgFe]﹩{}^{{\prime} }﹩ (left) Mgb vs. 〈Fe〉 (right) diagrams for NGC 3182 from center to outskirt with TMB model grids for ages, metallicities, and abundance ratios. The line strengths are measured along annuli. Symbol sizes are proportional to the radius. The regions of the star-forming ring (3″–8″) are enclosed with violet circles. In the Mgb vs. 〈Fe〉 diagram, solid and dashed lines are the 10 Gyr and 2 Gyr models, respectively. The model lines of [Z/H] = 0 in the right panel are emphasized as thick lines for each age. Each error bar indicates the measurement uncertainties in each annulus.
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: Age, metallicity, and α-abundance profiles. Filled symbols are from the measurement of lick indices absorption line strengths with the measurement uncertainties on each point are shown. Open symbols are from the measurement of mass-weighted age and metallicity by full spectral fitting using pPXF, the error bars of which connect the maximum and minimum values measured from individual spaxels within each annulus. The vertical lines indicate the inner and outer boundaries of the star-forming ring.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: The left two columns are radial velocity and mass difference distribution of north minus south sides in the R (or L  Z ) and V  ϕ  plane, right two columns are the ridge difference at different age populations, which are helpful for one to find the time-evolving ridge.
Paper: Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars
Authors: Peng Yang, Hai-Feng Wang, Zhi-Quan Luo, Thor Tepper-García, Yang-Ping Luo
Figure caption: Radial velocity distribution on the R and V  ϕ  plane and the rotational (azimuthal) velocity is overlapped with black curve. Note that the rotation curve has slight wobble near the ridge region indicated by the vertical dashed lines.
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: In the left, the SDSS g, r, and ibands composite image (130″ × 130″) of NGC 3182 galaxy. In the right, the zoom-in image of the central 50″ × 50″ (white box in the left column). North is to the top and east is to the left.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The upper panel: the single exposure spectra of J2240 from LAMOST and P200. The spectra from bottom to top are in phase ascending order, and adjacent spectra are shift by 0.5 in y direction to make a clear view. The phases are shown in the right side. Details are shown in Table 1. The middle panel: the combined spectrum of the blue band (dark gray), overplotted with its best-fitting template (red). The lower panel: the residual in the fitting of combined spectrum of the blue band.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: Folded RV curves and LCs in different bands (V band of Catalina, g, r, and i bands of ZTF) with a period of 0.219658 days. The phases of quadratures (ϕ = 0.25 and 0.75) and inferior conjunction ϕ = 0.5 are marked with vertical gray lines. A calculated RV curve is shown using best-fit K1 = 318.5 km s−1 and V sys = −68.6 km s−1.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The the SED fitting of J2240 with single component. The red dots denote observations used for fitting, including GALEX, SDSS u, the PS1, VISTA, and WISE observations. The model parameters are T eff = 7360 K, log g = 4.43 and [Fe/H] = 0.08, and the E(B − V) is 0.055. The residuals are expressed as ((Observed − Calculated)/Observed, and the vertical lines denote the error.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The corner plot of SED fitting results of J2240 with single component. The KURUCZ model is used, while observations include GALEX, SDSS u, PS1, VISTA, and WISE W1. See text for details.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The Lomb–Scargle Power for the combined light curves of ZTF g, ZTF r and Catalina V. The power peaks at half orbital period (0.109829 days), with FWHM ≈ 0.000002 days.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Top Individual transits from TESS from sectors 5 and 13 at 30 minute cadence and from sectors 30 and 38 at 2 minute cadence. The red circles indicate the measured data for sectors 5 and 13 and the binned data at 30 minute cadence for sectors 30 and 38. The 2 minute cadence data for sectors 30 and 38 are plotted as brown points. The best-fit model, incorporating the transit-timing variations in Section 4, and out-of-transit trends are shown by the red lines. Bottom left: the phase-folded TESS transit and best-fit model. Bottom right: the combined follow-up LCOGT 1 m observations from 2022 January 3 in the ﹩i^{\prime} ﹩ band.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: TESS light curve (brown) of TOI-4562b from all 25 available sectors. Photometry prior to sector 13 was obtained at 30 minute cadence, while latter observations were obtained at 2 minute cadence and binned in this figure to 30 minutes for clarity. The four TOI-4562b transits from Sectors 5, 13, 30, and 38 are marked by red arrows. The host star exhibits up to ∼3% peak-to-peak stellar rotational modulation due to its youth.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Observed—calculated midtransit time for the five transits of TOI-4562b, in minutes. The second and third transits (from TESS Sectors 13 and 30) show a ∼20 minute midtransit time difference with the other transits, suggesting the presence of a third body in the system.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Flow chart of the TESS_localize method described in this work. The first gray box and the green diamonds are the only parts of the software that require user input.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Heatmap plots of flux (top) and best-fit amplitude (bottom) for three eclipsing binaries observed by TESS (Prša et al. 2022). From left to right, these data are for targets TIC 269697721 (Sector #24), TIC 133105082 (Sector #7), and TIC 380784511 (Sector #17). In all images, the target star is marked by a red “X,” the localized signal is marked with a black “X,” the target aperture is boxed in red, and the stars in the TPF are marked in gray. Left: example of a TESS_localize fit where the target star was found to be the star exhibiting the binary eclipsing signal. This is the type of fit that is captured in the Gaussian statistics of our GMM model. Middle: TESS_localize fit where the target star has a low CROWDSAP, and is not the star found to be exhibiting the binary signal. Right: TESS_localize fit where the target star has a high CROWDSAP, and is not the star found to be exhibiting the binary signal.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Residuals between the fit locations and the known locations of the targeted stars. The top and right panels display marginalized histograms, and the dashed lines show the marginalized two-component Gaussian mixture model that we adopt as an extrinsic error model in Section 4.2.1.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Subpixel best-fit locations for 9774 binary stars. The top and right panels display marginalized histograms. Excesses at every ninth of a pixel, as well as at the edge of pixels (0.5) indicate that the procedure of fitting a PRF model to data prefers these locations.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: DESI CCD image layout with four amplifiers. The CCD images for all cameras have the same orientation after transformation of the data array by the instrument control system; the column index (AXIS1 in the fits files headers, often labeled X in this paper) increases with the fiber number, and the row index (AXIS2 in fits, often label Y in this paper) increases with increasing wavelength. The black arrows indicate the direction of readout, with the parallel clock in the wavelength direction (Y) and the serial clock along the fiber number (X). Also shown are the prescan and overscan regions used to measure and remove the bias level during pre-processing (see Section 4.2).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Spectroscopic pipeline data flow.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Example CCD image after pre-processing. This is an NIR CCD image of spectrograph SM10 after a 900 s exposure. On the top panel, one can see the 500 fibers organized in 20 blocks of 25 fibers each. The mostly horizontal curved lines are sky lines. Bright fibers (appearing as vertical dark bands in this negative color scale) are the spectral traces from standard star fibers. One can also note many cosmic-ray hits. The lower panel is a zoom highlighting the clear separation of the fiber traces, the space between blocks, and the spectrograph resolution (see Section 4.3 for more details on the resolution).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: A 200 × 200 pixel region of a dark image from the red camera of spectrograph SM6, without and with the negative trail correction. Note the bright trails corresponding to negative values in this inverted gray scale on the left of cosmic-ray hits on the left panel. The serial clock moves charges to the right in this region of the CCD read with amplifier B.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Photon transfer curve for spectrograph SM5, camera r, amplifier C, obtained with pairs of exposures of 1, 2, 5, 10, 20, and 50 s with the LED lamps illuminating the dome screen. The units on the figure are ADU (or ADC counts). A gain of 1.509 electron per ADU is determined from the inverse of the slope.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Schematic view of one of the 10 DESI spectrographs. See text for details.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Illustration of the DESI calibration system with the location of the screen and calibration lamps. The diameter of the dome screen is 5 m.