adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The top, middle, and bottom panels show the in situ observations of the total magnetic field, the speed of the solar wind, and the proton density, respectively, as obtained by Wind during the ICME Event 6. The two red dashed lines mark the boundary of the MC. The blue-shaded region followed by the MC marks the location of the HDS.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The black solid lines within the boundary marked by the vertical red lines, denote the magnetic vectors (in SCEQ coordinates) of the ICME which is sequentially observed by MESSENGER and WIND for Event 6. The gray-shaded regions are the model results obtained for Run1. The cyan and magenta colored dashed lines in the right panels denote the model results for Run2 and Run3, respectively.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Experiment II: reconstructions results of the radio galaxy 3C 353. The first and third rows show the ground-truth image and the estimated images obtained by the imaging algorithms (logarithmic scale). The second and fourth rows show the dirty image and the corresponding residual dirty images (linear scale). For R3D3, we showcase the results of its realization with J = 6 layers in its R2D2-Net components. Values of (S/N, log S/N) are reported below estimated images. The ﹩{\overline{\sigma }}_{{\rm{res.}}}﹩ values are indicated below the residual dirty images.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Experiment I: reconstructions results of the galaxy cluster A2034. The first and third rows show the ground-truth image and the estimated images obtained by the imaging algorithms (logarithmic scale). The second and fourth rows show the dirty image and the corresponding residual dirty images (linear scale). For R3D3, we showcase the results of its realization with J = 6 layers in its R2D2-Net components. Values of (S/N, log S/N) are reported below estimated images. ﹩{\overline{\sigma }}_{{\rm{res.}}}﹩ values are indicated below the residual dirty images.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Illustration of the R2D2 algorithm. Both image iterates  x  (i−1) and associated residual dirty images  r  (i−1) are fed to R2D2 DNNs as input. R2D2 DNNs’ output is then used to update the next image iterates. The sequence of the image iterates and corresponding residual dirty images are indicated with dashed red and green arrows, respectively. The sequence of the learned residual images is indicated with blue arrows.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Illustration of the U-Net core architecture underpinning the different incarnations of the R2D2 algorithm. The convolutional layers of the network, represented as boxes, apply multichannel convolutions, followed by down-sampling (contracting path) or up-sampling (expanding path). The outcome of these layers are 3D feature maps, whose dimensions are specified around the corresponding boxes: the 2D spatial dimension at the bottom center, and the number of feature channels at the outer edge.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Selection of raw low-dynamic-range images (linear scale; top row), and corresponding ground-truth images after preprocessing (logarithmic scale; bottom row). The training data set includes medical images (first column), and optical astronomy images (second column). The validation data set comprises images of giant radio galaxies (e.g., Messier 87; third column), and radio galaxy clusters (e.g., A746; fourth column).
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Selection of simulated 2D Fourier sampling patterns with the antenna configuration of the VLA (top row) and resulting dirty images (linear scale; bottom row). The depicted dirty images correspond to the ground-truth images shown in Figure 3.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Progress of the reconstruction quality (left column: S/N, middle column: log S/N) and data fidelity (right column: ﹩{\overline{\sigma }}_{{\rm{res.}}}﹩) across the iterations of R2D2 and both realizations of R3D3. Values of the different metrics, achieved at convergence by the benchmark algorithms uSARA, AIRI, and CLEAN, are reported via horizontal lines. From top to bottom: results of Experiments I–IV. In each scenario, the reported values are averages over a test data set composed of 100 inverse problems.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Results of the data set pruning procedure. Evolution of the size of the training data set shown as a fraction of the size of the initial training data set, throughout the iterations of R2D2 and both R3D3 realizations (R3D33L, R3D36L).
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Color–color diagrams for the PHANGS-HST human-classified sample, with each morphological class shown separately: C1 single-peaked symmetric clusters (left column); C2 single-peaked asymmetric clusters (middle column); and C3 multipeaked compact associations (right column). In all panels, V − I is plotted along the horizontal axis, and three other colors are shown along the vertical axis: NUV-B (top row), U − B (middle row), and B − V (bottom row). We only show data points for clusters that are detected with at least an S/N > 3 in the plotted bands. Individual clusters are represented by black dots whereas in crowded regions we show a Gaussian-smoothed heat map indicating the relative density. The size of the smoothing kernel is shown by a red circle on the top middle panel. A cyan track denotes the BC03 SSP model for Z ⊙ metallicity at ages from 1 Myr until 13.7 Gyr. The portion of the SSP track Z ⊙/50 metallicity from 0.5 to 13.7 Gyr is also shown with a magenta track. Key ages are indicated on the right column and are marked with blue and pink dots on each track. A reddening vector (top right of each panel) corresponds to A  v  = 1.0 mag. In panel (d), we indicate names for relevant loci in the color–color space.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Probability distributions of apparent total V-band magnitude (i.e., corrected for aperture losses) for the cluster (class 1 + 2) and compact association (class 3) populations in all 38 PHANGS-HST galaxies. We show with red (gray) the human- (ML) classified catalogs. In order to compare their distribution, we normalized the histograms to the highest bin of the ML sample. For each target, we display the distance and the faintest detected magnitude for the human and the ML-classified clusters. A gray dashed line shows the median ML V-band magnitude, and the solid black line the limit of M  v  = −6 used as the lower magnitude cut in Adamo et al. (2017). We mark targets with a star, if the faintest human detected magnitude is brighter than the median ML detected magnitude.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Color–color diagrams for the human cluster sample (top row) and the ML cluster sample (middle and bottom rows). In the middle row, we show all ML-classified clusters, whereas the bottom row only shows ML-classified clusters up to the same V-band magnitude for each target as detected for the human sample. The individual V-band cuts are estimated with the maximal detected magnitude as presented in Figure 2. Cluster classes 1, 2, 1 + 2, and 3 compact associations are shown individually in each column from left to right, respectively. Clusters are represented by black dots and in crowded regions by a Gaussian-smoothed heat map indicating the relative density.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: The number of star clusters (top panel) and compact associations (bottom panel) in each of the 38 PHANGS-HST galaxies, shown as a function of the specific star formation rate (sSFR), estimated inside the HST footprint. Sources that have been inspected and classified by a human (co-author B.C.W.) are shown in dark green, while those that have been classified using a neural network model (Hannon et al. 2023) are shown in light green.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Absolute V-band magnitude (top panels) and stellar mass (bottom panels) as function of galaxy distance. The left (respectively right) panels are for human- (respectively ML) classified star clusters (class 1 + 2) for each galaxy. Gray dots with error bars denote the median value and the 16–84 percentile range, red (respectively blue) dots represent the brightest (respectively faintest) V-band magnitude. The most (respectively least) massive clusters are shown with violet (respectively green) dots. In the top left panel, we use open circles, if the maximal human detected magnitude is brighter than the median ML detected magnitude (see Figure 2).
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Distribution of the absolute V-band magnitude of the human (red) and the ML (gray) samples for class 1 + 2 + compact associations shown as dotted lines in all three panels. To visualize individual cluster classes, we show their distributions with solid lines in each panel. The histograms are shown in logarithmic scale to visualize the zone where both samples have comparable sizes, as well as the differences when the machine-learning sample size increases toward fainter magnitudes.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Mean color uncertainties for the NUV-B vs. V − I (top row) and U − B vs. V − I (bottom row) diagrams. We present class 1 + 2 clusters for ML (left two panels) and human classifications (right two panels) separately. The maps show the mean uncertainty in each bin, and only bins with at least five clusters are displayed.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: The brightest (absolute V-band magnitude, uncorrected for internal extinction) cluster in each PHANGS-HST target. Color images are constructed from I-, V-, and U-band data, and each cutout spans 2.″38 (corresponding to ∼50–270 pc, depending on the distance to each galaxy). The clusters are arranged from left to right, top to bottom in the order of Table 3.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The evolution of a top-hat jet with a half-opening angle of 0.1 radians traveling in a constant density interstellar medium. Different phases of the jet are represented by the corresponding colors: blue lines the coasting phase, green lines the deceleration phase, orange lines the spreading phase, and red lines the Newtonian phase. Left-hand panel: normalized energy. Middle panel: proper velocity. Right-hand panel: radius scaled with R(θ = 0).
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The coefficients to calibrate our method with Blandford–McKee and Sedov–Taylor self-similar solutions.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: A comparison between jetsimpy and the numerical hydrodynamic code JET. The numerical setup is a top-hat jet with a half-opening angle of 0.052 radians (3 degrees) traveling in a uniform external medium. We present a comparison of three stages during the evolution: the blue lines that represent the initial condition, the green lines that represent the intermediate stage of spreading, and the red lines that represent the Newtonian phase.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The evolution of proper velocity for isotropic explosion with various initial Lorentz factors (γ 0 = 10, 100, and 1000 for green, orange, and blue lines, respectively). The time is scaled by r 0/c, which is the time when the jet becomes subrelativistic. The dashed lines are the exact Blandford–McKee and Sedov–Taylor self-similar solutions.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: The upper panels show distributions of galaxy properties of the galaxy pair sample and the control sample, while the lower panels present the offset of these properties relative to the controls. The paired galaxies and control galaxies are plotted as filled and open histograms, respectively. The dashed lines represent the mean value of distributions for paired galaxies. (a) Distributions of ﹩{f}_{{{\rm{H}}}_{2}}﹩. (b) Distributions of sSFR. (c) distributions of SFE. (d) Distributions of ﹩{\rm{\Delta }}{f}_{{{\rm{H}}}_{2}}﹩. (e) Distributions of ΔSFR. (f) Distributions of ΔSFE.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: Global SFR as a function of stellar mass. The blue circles represent galaxy pairs selected from the MaNGA survey, while the gray squares are isolated galaxies from the control sample. From top to bottom, the three dashed lines correspond to log(sSFR yr−1) = −9.5, −10.5, and −11.5.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: The left panel shows the distributions of redshift for the galaxy pair and the control sample. The right panel shows the distributions of stellar mass for the galaxy pair and the control sample.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: The upper panels show histograms of different galaxy property offsets. The lower panels show the corresponding mean values for the offset distributions. In each plot, paired galaxies at different merger stages and the control sample are marked with blue, orange, red, and black, respectively. In the lower panels, the mean value of each distribution is indicated by a square point, and the error bar represents the standard error of the mean for each distribution. (a) The distribution of Δf gas. (b) The distribution of ﹩{\rm{\Delta }}{M}_{{{\rm{H}}}_{2}}﹩/M H I . (c) The distribution of ΔSFEgas. (d) The mean value of Δf gas. (e) The mean value of ﹩{\rm{\Delta }}{M}_{{{\rm{H}}}_{2}}﹩/M H I . (f) The mean value of ΔSFEgas.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: The upper panels show histograms of different galaxy property offsets. The lower panels show the corresponding mean values for the offset distributions. In each plot, paired galaxies at different merger stages and the control sample are marked with blue, orange, red, and black, respectively. In the lower panels, the mean value of each distribution is indicated by a square point, and the error bar represents the standard error of the mean for each distribution. (a) The distribution of ﹩{\rm{\Delta }}{f}_{{{\rm{H}}}_{2}}﹩. (b) The distribution of ΔSFR. (c) The distribution of ΔSFE. (d) The mean value of ﹩{\rm{\Delta }}{f}_{{{\rm{H}}}_{2}}﹩. (e) The mean value of ΔSFR. (f) The mean value of ΔSFE.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: The upper panels show distributions of galaxy properties of the galaxy pair sample and the control sample, while the lower panels present the offset of these properties relative to the controls. The paired galaxies and control galaxies are plotted as filled and open histograms, respectively. The dashed lines represent the mean value of distributions for paired galaxies. (a) Distributions of the total gas fraction f gas. (b) Distributions of molecular-to-atomic gas mass ratio ﹩{M}_{{{\rm{H}}}_{2}}﹩/M H I . (c) Distributions of the SFE of the total gas SFEgas. (d) Distributions of Δf gas. (e) Distributions of ﹩{\rm{\Delta }}{M}_{{{\rm{H}}}_{2}}﹩/M H I . (f) Distributions of ΔSFEgas.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: CO(2−1) spectra of the detected galaxies from IRAM 30 m observations. Most of the spectra were rebinned to a velocity resolution of ∼20 km s−1, and some spectra were rebinned to a velocity resolution of ∼40 km s−1 to achieve detections. The velocity of each spectrum is Doppler corrected and converted to the barycentric frame, and the zero-point is set based on the optical spectroscopy redshift of the galaxy.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: CO(1−0) spectra of the detected galaxies from IRAM 30 m observations. Most of the spectra were rebinned to a velocity resolution of ∼20 km s−1, and some spectra were rebinned to a velocity resolution of ∼40 km s−1 to achieve detections. The velocity of each spectrum is Doppler corrected and converted to the barycentric frame, and the zero-point is set based on the optical spectroscopy redshift of the galaxy.
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: CO(2−1) spectra of the detected galaxies from JCMT observations. Most of the spectra were rebinned to a velocity resolution of ∼10 km s−1, and some spectra were rebinned to a velocity resolution of ∼20 km s−1 to achieve detections. The velocity of each spectrum is Doppler corrected and converted to the barycentric frame, and the zero-point is set based on the optical spectroscopy redshift of the galaxy.