adsabs/AstroCLIMB huggingface dataset:
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Example of stray light analysis and mitigation. Left: PST comparing the scatter from nonblack paints on the center section to black paints. Right: the Mayall telescope center section before painting any part black. Repainting the center section black reduces its contribution to scattered light by an order of magnitude. This in turn reduces the total stray light across all input angles in the left panel: the reduction in stray light integrated over all angles is significant. (Images previously published in Miller et al. 2016b.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Hexapod actuator accuracy test. The hexapod vendor tested the displacement of an actuator with flexures by commanding the actuator to a series of positions. The plot compares the commanded position, the position measured by an internal encoder, and the position measured by an external device. The differences are well within requirements.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: The ADC rotator. The rotator is shown being aligned in the Middle section of the barrel using a CMM at FNAL. The ADC1 and ADC2 lens cells are visible in the inner diameter. One of the two custom bearings between the cells and barrel is visible in the lower left corner.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Schematic of the pencil laser beam alignment system successfully used for the DECam corrector. The DESI system was identical to this one. (Image previously published in Brooks et al. 2016.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: The ADC rotator.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Available space to accommodate the ADC1 and ADC2 rotation mechanisms.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Measured PSF FWHM image quality as a function of zenith angle. Approximately 480,000 guider camera images contribute to this plot; the grayscale areas show the density of data points binned by zenith angle and difference between each observation’s FWHM and the corresponding nightly median FWHM. The moving median trend of Mayall/DESI image quality vs. zenith distance (red line) remains quite flat until around 50°−60°, as expected from the optical design. The corresponding Mayall/MOSAIC trend (blue line) is very similar. The dashed magenta line denotes average image quality independent of zenith distance. (Image previously published in Meisner et al. 2020.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Measurement of the delivered image quality of the corrector. Left: radial profile of the star on a night with superb seeing (0.″57 on 2019 April 3). Right: histogram of FWHM measurements from approximately 480,000 r-band images obtained during the DESI Commissioning phase, 2019 October−2020 March. The median FWHM is 1.″11, consistent with the expected performance of the corrector and with the pre-DESI performance of the MOSAIC prime focus camera. (Right image previously published in Meisner et al. 2020.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Examples of scattering inside the barrel. Left: model of scatter from flat surfaces on C2 and ADC2 lens cells. For a particular input angle, the incoming rays (from the left) were scattered at the lens edges (labeled by the black arrows), sending diffuse light toward the focal surface. These scatter sources were mitigated by adding fine grooves to the flange surfaces. Right: model of scatter from the hexapod mounting flange inside the corrector barrel. For a particular input angle, the incoming rays (from the left) were scattered by the flange (labeled by the black arrow), sending diffuse light toward the focal surface. Low baffles immediately past the flange were added to block the scatter. (Images previously published in Miller et al. 2016b.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Image of the galaxy M51 obtained on 2019 April 1, the first night of observations with the corrector. This image was obtained with the DESI CI through an r-band filter with the CCD camera at the center of the field of view. The image quality in this observation was approximately 0.″65 FWHM. The field of view of one of the CI CCDs is approximately ﹩6.7^{\prime} \times 4.4^{\prime} ﹩. North is up and east is to the left in the image.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Corrector assembly at Kitt Peak. Left: the Aft and Middle barrel sections being reassembled on the UCL precision turntable on the Mayall ground floor for post-shipment alignment verification. Right: the fully assembled corrector barrel and hexapod being lifted by the Mayall dome crane from the integration stand on the ground floor to the cage/vanes/ring assembly on the C floor in the Mayall dome. (Images previously published in Besuner et al. 2020.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Shipping fixtures. Left: model of C2 lens in its dedicated shipping fixture. Right: the Mid barrel segment being unloaded at Kitt Peak; the segment is secured in an aluminum frame and rests on wirecoil isolators on its crate base.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Integration of the top end. Left: top end being lifted by crane. Right: top end installed on Mayall telescope trusses. (Right image previously published in Besuner et al. 2020.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: The corrector and hexapod installed in the cage and upper ring located in the Mayall dome. The corrector has been centered relative to the upper ring. (Image previously published in Besuner et al. 2020.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Image of a star before (left) and after (right) mirror edge mask installation. The mask blocks the outer edge of the primary mirror, where there are polishing errors, and thus removes smear in the image. The image was captured on a CI CCD and is overexposed to show the dimmer outer region of the PSF; the bright central core is blacked out in the image.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Left panel: Color-composite image (red: WISE 22 μm; green: WISE 12 μm) of present 1° × 1° target area. Right panel: 12CO peak intensity map of the selected region. The blue and red contours represent the 12CO m-0 contours for the northern and southern molecular structures/clouds, respectively (see Section 4.1). The lowest level value for both the contours is the mean value with a step size of 1σ. The locations of five sites of active star formation are also marked with a magenta “+” marker in both panels.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Channel maps for 12CO (J = 1 − 0) emission integrated over marked velocity interval in each panel (in  kilometers per second). The emission is depicted above the 5σ value (σ being the rms noise). The “+” magenta markers depict the clusters’ locations.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Upper left panel: 12CO (J = 1 − 0) m-0, and lower left Panel: 13CO (J = 1 − 0) m-0 maps overlaid with elected locations (N1—N4) to extract spectra and red colored path to extract the PV diagram in the velocity range [−22, −12] km s−1 for northern molecular cloud along with YSOs (Class I (yellow asterisk) and Class II (green asterisk)). Right Panel: 12CO (J = 1 − 0; blue color) and 13CO (J = 1 − 0; red color) spectra at the selected locations marked in the left panel. The green and yellow curves represent the Gaussian fit/s to these spectra. The vertical dashed (blue) line represents the 12CO Gaussian fit/s peak.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Upper left panel: 12CO (J = 1 − 0) m-0, and lower left panel: 13CO (J = 1 − 0) m-0 maps overlaid with elected locations (S1—S4) to extract spectra and red colored path to extract the PV diagram in the velocity range [−4, 6] km s−1 for KPS0620 along with YSOs (Class I (yellow asterisk) and Class II (green asterisk)). Right panel: 12CO (J = 1 − 0; blue color) and 13CO (J = 1 − 0; red color) spectra at the selected locations marked in the left panel. The green and yellow curves represent the Gaussian fit/s to these spectra. The vertical dashed (blue) line represents the 12CO Gaussian fit/s peak.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: PV diagram generated using 13CO emission, along the path (red vectors) overlaid in Figure 4 for the northern molecular structure. The orange straight lines represent the prominent peak 13CO emission of −18.1 km s−1 and −18.7 km s−1 in the direction of locations N1 and N3, respectively (see Figure 4).
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Left panels: Herschel column density map overlaid with the locations of Class I (yellow asterisk) and Class II (green asterisk) YSOs. Middle panels: Herschel temperature map. Right Panels: Spitzer ratio map (4.5 μm/3.6 μm emission) for KPS0620 (upper panels) and IRAS 05331+3115 (bottom panels).
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Left panels: Herschel column density map overlaid with the locations of Class I (yellow asterisk) and Class II (green asterisk) YSOs. Middle panels: Herschel temperature map. Right Panels: Spitzer ratio map (4.5 μm/3.6 μm emission) for AFGL 5157 (upper panels) and FSR0807 (bottom panels).
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: m-0, m-1, and line-width maps (column-wise) for 12CO (J = 1 − 0) and 13CO (J = 1 − 0) emission, respectively, in the velocity range [−22, −12] km s−1 for the northern molecular cloud. The emission is depicted above the 5σ value (σ being the rms noise for respective spectral cubes).
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: m-0, m-1, and line-width maps (column-wise) for 12CO (J = 1 − 0) and 13CO (J = 1 − 0) emission, respectively, in the velocity range [−4, 6] km s−1 for KPS0620. The emission is depicted above the 5σ value (σ being the rms noise for respective spectral cubes).