adsabs/AstroCLIMB huggingface dataset:
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: The data from Figure 2 expanded into separate panels for each galaxy. Logarithmic medians are presented within each panel. While there are galaxy-to-galaxy differences, the overall sample shows no significant differences between the medians and dispersions for clusters and associations.
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: A box and whisker plot of the data from Figure 2 as a function of stellar cluster age. The y-axis values for each age bin are the median ratios normalized by the median diffuse value. The horizontal bars within each box indicate the median values, the boxes themselves span the 25th–75th percentiles, and the whiskers span the 10th–90th percentiles. Linear fits to the data have Spearman's rank correlation coefficients ranging between −0.833 and −0.950 and two-sided significance levels of their deviations from zero ranging between 0.001 and 0.005.
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: All 19 Cycle 1 PHANGS–JWST galaxies as seen by the JWST/MIRI F770W filter. Small white circles indicate the locations of stellar clusters for which we study PAH feature ratios. Large blue circles indicate 200 pc diameter diffuse regions that do not overlap with stellar clusters, stellar associations, or H II regions and serve as a control sample in the analysis. Horizontal scale bars indicate 1 kpc.
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: Similar to Figure 2, but after removing the hot dust continuum levels for F770W and F1130W.
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: Similar to Figure 3, but after removing the hot dust continuum levels for F770W and F1130W.
Paper: PAH Feature Ratios around Stellar Clusters and Associations in 19 Nearby Galaxies
Authors: Daniel A. Dale, Gabrielle B. Graham, Ashley T. Barnes, Dalya Baron, Frank Bigiel, Médéric Boquien, Rupali Chandar, Jérémy Chastenet, Ryan Chown, Oleg V. Egorov, Simon C. O. Glover, Lindsey Hands, Kiana F. Henny, Remy Indebetouw, Ralf S. Klessen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daniel Maschmann, Debosmita Pathak, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Tony D. Weinbeck, Bradley C. Whitmore, Thomas G. Williams, Aida Wofford
Figure caption: Similar to Figure 6, but after removing the hot dust continuum levels for F770W and F1130W.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Shared axis plots for the GAGDR3 sample. The center plot is the H-R diagram in MG vs. BP − RP. The three thin red lines mark the general distribution of the main sequence. The top and bottom red lines mark the envelopes of the main sequence, and the center red line is the best-fitted line for the main sequence. The thick angled red line indicates the top edge of the main-sequence gap. All these red lines are defined empirically in W.-C. Jao et al. (2023). Stars above the gap have a partially convective interior, and stars below the gap are fully convective. The top and bottom plots are the H-R diagram plotted in absolute NUV and FUV magnitudes, respectively. The left and right plots are the absolute G magnitudes against the absolute NUV and FUV magnitudes, respectively. The vertical and horizontal colored boxes indicate the approximate range of the main-sequence gap. The blue dots connected in a blue line in the left plot are the numbers of stars within a bin size of MG = 0.2 mag. Three spectral types are labeled at their approximate positions. The two populations of M dwarfs are on self-defined “upper” and “lower” branches in the left plot, and we will mention these two terms throughout this work.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Magnitude limits of GALEX at various distances. The top two plots show the apparent magnitudes in NUV and FUV for our sample (black dots) against distances. The two red dashed lines mark the approximate GALEX apparent magnitude limits at 23.4 and 22.9 mag for the NUV and FUV bands, respectively. The bottom four plots show the absolute magnitude limits in the NUV and FUV bands at various distances, marked by the shaded gray boxes, and the absolute magnitude limits are given in Table 1. The blue dots are stars with distances between 50 and 100 pc, and the red dots represent stars within 50 pc.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Color–color diagrams with NIRCam 3–5 μm medium-band filters. Companions, namely the HR 8799 planets, the field-age brown dwarf companion HD 19467 B (A. Z. Greenbaum et al. 2023; K. K. W. Hoch et al. 2024), and the young companion VHS 1256 b (B. E. Miles et al. 2023) are illustrated in black. Also shown in black are the two field L-dwarfs targeted by GO 2288 (PI: J. Lothringer); the BD labeled “#1” is 2MASSW J2148162+400359, and “#2” is 2MASS J06244595-4521548. The AKARI sample of L-T field brown dwarfs (S. Sorahana et al. 2013) and the JWST sample of late T- and Y-dwarfs (S. A. Beiler et al. 2024) are colored by their spectral type. Over plotted are cloudless Sonora-Bobcat evolutionary models (M. S. Marley et al. 2021) at 1 Gyr (solid) and 30 Myr (dashed) for solar metallicity (blue) and enhanced metallicity (orange). A number of qualitative features are noticeable, (1) the HR 8799 planets are offset toward bluer F430M – F410M colors than the field sample, corresponding to the younger and more metal enhanced evolutionary model tracks, (2) the planets show significant spread across the diagram despite their apparently similar photometric colors in the NIR (see, e.g., Figure 1 in M. Bonnefoy et al. 2016), and (3) there is an apparent sequence, from the inner planet HR 8799d to the outer planet HR 8799b in F460M – F410M color.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Planet locations per roll angle in detector coordinates at the epoch of observation, compared to the idealized coronagraph transmission function of the NIRCam LWB/narrow offset position. Left panel: illustrating the position of the four HR 8799 planets in program 1194. Right panel: illustrating the position of 51 Eri b in program 1412. The first roll angle position is indicated with blue circles, the second with red squares, and the legend indicates the position angle of the telescope aperture for each roll. Takeaway: This figure also explains the difference in our forward modeling analysis for each system. In the 51 Eri observations, the coronagraphic throughput at the location of the faint planet does not change significantly between roll angles, and we opt to forward model the planet simultaneously in both roll angles using an ADI+RDI starlight subtraction. In the HR 8799 observations, the coronagraphic throughput at the location of the relatively brighter planets changes significantly between roll angles, and HR 8799 e suffers from strong self-subtraction due to the orientation of the position-dependent PSF and the roll angle, motivating a roll-by-roll forward modeling analysis with an RDI starlight subtraction.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: LWB/narrow observations of all four HR 8799 planets (SW filters as blue hexagons, LW filters as gold hexagons) compared to the ground-based observations of the planets collated by E. Nasedkin et al. (2024) and used in their retrieval analysis (data from C. Marois et al. 2008; M. Fukagawa et al. 2009; C. Bergfors et al. 2011; R. Galicher et al. 2011; S. Esposito et al. 2013; Q. M. Konopacky et al. 2013; T. Currie et al. 2014; A. J. Skemer et al. 2014; T. S. Barman et al. 2015; A. L. Maire et al. 2015; A. Z. Greenbaum et al. 2018; GRAVITY Collaboration et al. 2019; D. S. Doelman et al. 2022; J. J. Wang et al. 2022; E. Nasedkin et al. 2024). A comparison with their models can be found in Appendix C, Figure 15. Our measurements show agreement with ground-based L- and M-band observations to within 1σ−2σ. There is tension in the K band between our observations at F182M, F200W, F210M, and F250M and the VLTI/GRAVITY spectra, especially of HR 8799c and HR 8799d. This could be due to the absolute flux calibration of the VLTI/GRAVITY spectra; see discussion in Section 4.1. The variation in 3–4 μm and 4–5 μm slopes between each planet indicate unique photospheric abundances of CH4, CO, and CO2, as discussed in Section 5.1.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Imaging Summary. Left panel: PSF-subtracted F410M image of HR 8799, pyKLIP subtraction parameters labeled to the top right. Middle panel: same as left panel, but zoomed in to 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 by 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0, and the outer three planets have been forward modeled and subtracted, leaving HR 8799 e visible. See also the deconvolved image of HR 8799 in this filter in Appendix B, Figure 14. Right panel: PSF-subtracted F410M image of 51 Eri b, showing the detection of the planet at its expected location.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam F410M 5σ contrast curves for the LWB/narrow coronagraph (solid black line) and the 335R coronagraph from (dashed black line; A. L. Carter et al. 2023) The turnover in contrast performance between the two modes occurs at about 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩75 (just outside of the IWA for the MASK335R). Our detections of the four HR 8799 planets, recorded in Table 2, are shown with their associated contrast uncertainty as an error bar inset within their scatter points. The wedge mask outperforms the round mask at close separations (<0﹩\mathop{.}\limits^{^{\prime\prime} }﹩7) thanks to its sharper inner working angle and higher throughput, but suffers at longer separations. The LWB/narrow mode achieves C4.1 μm = 10−4 at 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩33 at 5σ.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Model of the idealized 2D transmission function for the band-limited NIRCam MASKLWB coronagraphic mask in detector coordinates, generated using webbpsf. For each point in the detector frame, filter-dependent offsets are indicated by crosses and labeled, including the “narrow” offset position.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: SED of 51 Eri b and best-fitting Exo-REM models. The top panel illustrates the transmission functions for each photometric filter. The middle panel shows the GPI (black circles; B. Macintosh et al. 2015; A. Rajan et al. 2017) and SPHERE (black squares; M. Samland et al. 2017; S. B. Brown-Sevilla et al. 2023) low-resolution spectra of the planet, as well as ground-based ﹩L^{\prime} ﹩- and M-band photometry (blue squares; A. Rajan et al. 2017), and the measurements from this work (gold hexagon, for our F410M detection, and gold downward-facing triangles for our F335M, F430M, and F460M nondetections). Over plotted is the best-fitting Exo-REM model in magenta, and then 1σ, 2σ envelopes showing the range of accepted models. The bottom panel illustrates the residuals to the best-fitting model; there are noticeable residuals in the J-band GPI spectrum and the H-band SPHERE spectrum that could be related to speckle noise or instrument throughput. The fit shows good agreement to the ﹩L^{\prime} ﹩-band and F410M photometry, which constrain the CH4 and CO2 absorption slopes. The M-band photometry from A. Rajan et al. (2017) lies slightly above the best-fitting model, but in general is consistent with strong CO absorption due to vertical mixing.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Centering NIRCam LWB/narrow coronagraphic images. Left panel: first science frame from the HR 8799 observations in the F460M filter (the filter with the farthest distance between its typical filter-dependent offset and the narrow end of the wedge), in arbitrary pixel coordinates. The central leakage term is roughly centered, and the PSF wings appear about 20 pixels above and below this leakage; the field of diffraction peaks due to the edges of the Lyot stop are visible to either side of the bar, and are sensitive to the position of the star behind the coronagraph. Middle panel: webbpsf model PSF based on the nearest-in-time OPD observations, in arbitrary pixel coordinates. Right panel: overview of relevant positions in the padded 451  ×  451 pixel coordinates; the mask center for this filter is indicated by a blue cross, and the computed star position behind the mask is indicated by a red star.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: The orbit of 51 Eri b. Five-hundred randomly drawn orbits from our posterior distribution, determined using orbitize! in Section 4.2. Scatter points in blue represent literature relative astrometry, and those in red represent our new JWST/NIRCam measurement. The new detection agrees well with high-eccentricity (e = 0.58) solutions fit to previous observations.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption:                         Radial profiles of the normalized Hα flux, relative Hα RV, and flux ratios, color-coded by kinematic age. These curves are derived from the fitting results shown in Figures A1, A2, and A3. In the top left panel, the Hα flux is normalized to its value at r = 0.2rPDR. In the top right panel, the VLSR of Hα represents the relative velocity compared to the VLSR at r = 0.2rPDR. The ID number for each H II region is displayed alongside its corresponding curve. For curves that are difficult to distinguish, their ID numbers are grouped together and shown in parentheses.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Positions of the LAMOST fibers marked with circles, color-coded based on reddening E(B − V) derived from the Galactic 3D reddening map by G. M. Green et al. (2019). For clarity, the sizes of these fibers are enlarged, while the actual angular size (3﹩\mathop{.}\limits^{^{\prime\prime} }﹩3 in diameter) is shown as a black circle in the lower left corner. Green circles represent sizes of H II regions (rPDR) defined by the WISE catalog, while red circles indicate radii (rHα) derived from 1D Hα intensity profiles in this work. Background images are from WISE 12 μm observations.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Histograms of aperture size, physical size, expansion velocity, and kinematic age. The aperture size values, in units of arcminutes, are taken from the catalog by L. D. Anderson et al. (2014), while the other three parameters are derived in this work. The specific values for these parameters are listed in Table 1.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: A representative spectrum observed by LAMOST MRS-N. Nebular emission lines, including Hα, [N II], and [S II], are enlarged in the inset panels. The results of single Gaussian fitting are overplotted in red. As the spectrum is not flux-calibrated, the flux is given in units of ADU.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Relation between the escape fraction and kinematic age. The ID number for each H II region is enclosed within its corresponding open circle.