adsabs/AstroCLIMB huggingface dataset:
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: JCMT 850 μm continuum image overlaid with 13CO integrated intensity contours of different velocity components. They correspond to [5, 20], [40, 65], and [70, 85] km s−1. The rms levels (σ) of the four integrated intensities from (a) to (d) are σ 1 = 0.73 K km s−1, σ 2 = 0.72 K km s−1, σ 3 = 2.82 K km s−1, and σ 4 = 1.28 K km s−1, respectively. The red contour in each panel indicates the the 5σ level. The blue contour levels from panel (a) to (b) are [8σ 1, 10σ 1] K km s−1, [8σ 2, 10σ 2, 15σ 2] K km s−1, [10σ 3, 12σ 3, 15σ 3, 18σ 3, 20σ 3] K km s−1, and [10σ 4, 15σ 4, 20σ 4] K km s−1, respectively. According to the spatial association between gas and continuum emission, boundaries of different clouds are delineated by the black dashed lines. The beam size of 850 μm observations is also displayed at the bottom left corner of each panel.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Box plots of the physical properties: effective radius (a), mass (b), and mass surface density (c) for three classes of clumps (i.e., NFR, FR, and HR, see the text). The numbers within the parentheses in each classification indicate the number of clumps belonging to each class. The boxes represent the quartile range of the data, from the bottom to the top of each box, including the lower quartile (i.e., the 25th percentile), the median inside the box, and the upper quartile (i.e., the 75th percentile). The “whiskers” present the full extent of the data (i.e., minimum value and maximum value). The purple dashed line in panel (c) represents a mass surface density of 0.05 g cm−2. Scatter plots show the concentration of data, while whiskers represent the extent of data distribution. Different colored scatters mark the MSF clumps (MSFC) and non-MSF clumps (NMSFC).
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Mass–length diagram of individual filaments and hub-composing filaments within HFSs. The solid circles denote the individual filaments located at different distances, while the plus symbols mark the hub-composing filaments within HFSs. Numbers indicate hub-composing filaments characterized by notable deviations from the global trend (see text). The bold dashed–dotted line presents the relation L ∝ M 0.5 described by the simple model of Hacar et al. (2023). The thick dashed line at the top of the diagram represents a typical critical line mass of 16.6 M ☉ pc−1, while the bold dashed–dotted line represents the global trend between mass and length. The light dashed lines represent different reference line masses.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Box plots for comparison of mass surface density between clumps in an IR-dark environment (i.e., in Cloud 1 and/or Cloud 2) and those in an IR-bright environment (i.e., in Cloud 4). (a) Comparison between clumps in IR-dark Clouds 1 and 2 and those in IR-bright Cloud 4. (b) Distribution of mass surface density of HR clumps (i.e., those located at hubs) in both IR-dark (i.e., in Clouds 1 and 2) and IR-bright (i.e., in Cloud 4) environments. The numbers in parentheses of the horizontal axis labels represent the sample counts in each group.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Noise map and statistical histogram of the rms. Left: the color map presents the rms varying from 5 to 75 mJy beam−1 and the white contour indicates rms value of 20 mJy beam−1. The colored circles pinpoint three FOVs considered for analysis. Right: the histogram shows the distribution of the rms with a median value of 10 mJy beam−1 (red dashed line).
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Length and line mass distributions of filaments. The vertical blue line in both panels represents the median value, while the red line in panel (b) gives a critical line mass of 16.6 M ☉ pc−1.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Average spectrum of 13CO(1–0) emission over the G35 molecular complex. The colored bands highlight three major velocity components, corresponding to [5, 20], [40, 65], and [70, 85] km s−1 in green, red, and blue, respectively. The numbers represent the cloud IDs.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: An example of the averaged radial profile from the FILFINDER. The solid dark blue line shows the profile fitted with a Gaussian curve. Both 0.5 × beam size and 0.5 × FWHM are presented in the plot.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Distribution of parameters (i.e., FWHM, mass, column density) of filaments (blue) and clumps (orange). The corresponding median value is indicated with a vertical dashed line.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of upstream normalization constants with downstream values, all with units s3 km−6, and on logarithmic scales. Here and in subsequent figures, statistics are computed using a weighted least-squares evaluation of “fitted responses” ﹩{\hat{f}}_{l}﹩ with independent variable errors as weights w  l  (Equation (8)). p-Statistics, moreover, are given by one-way analysis of variance. Superimposed is a line representing parity between quantities (dashed line).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of upstream spectral indices with downstream values, given by model I (top panel) and model II (bottom panel).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of spectral indices given by DSA formalism with CfA compression ratios H                         ﹩\left(\gamma \equiv \tfrac{1}{2}\tfrac{3H}{H-1}\right)﹩, with fitted spectral indices yielded by model I (top) and model II (bottom).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of fitted rollover energies (model II) with those given by CfA measurements, per the functional form suggested in M. A. Lee (2005) or Equation (2). Here, the values of both θ  Bn  and γ are taken and calculated from the CfA measurements, respectively. Superimposed is a curve suggesting an inverse power relationship between the two quantities (dashed line), here ﹩{E}_{0}\propto {\left[(\sec {{\theta }_{{Bn}})}^{\tfrac{2}{2\gamma -3}}\right]}^{-1}﹩.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Fitted spectral e-folding energies per charge (E 0) and associated 1σ uncertainty errors (Equation (7)), with superimposed AAVSO solar activity (red axes). Here, the top panel shows the upstream rollover energies (blue, green, cyan), and the bottom panel shows the downstream energies (red, black, magenta), both for model II (Equation (6)).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of upstream rollover energies E 0 with downstream values within the range of the STICS sensor (6.2–223.1 keV/e) and regression statistics pertaining thereto as above.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Fitted spectral indices (γ) and associated errors with superimposed solar activity (red axes). Errors represent 1σ uncertainties σ  f  given by the L-M method (Equation (7)). sunspot numbers are tabulated in the Solar Bulletin publication by the AAVSO Solar Section. Moreover, the top panels designate upstream (blue, green, cyan) and downstream (red, black, magenta) indices obtained with model I (Equation (5)), while the bottom panels show γ values for model II (Equation (6)).
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of spectral indices given by model I (Equation (5)) with those given by model II (Equation (6)), the latter corrected to exclude γs associated with E 0 values beyond the WIND/STICS range.
Paper: Spectral Properties of Suprathermal Protons Associated with Interplanetary Shocks from WIND/STICS Data
Authors: Johann Rubens Mejia-Ott, Brent M. Randol
Figure caption: Comparison of fitted rollover energies with fitted spectral indices (model II). Here, the statistics were evaluated by taking the log of the rollover energies, with the spectral indices unchanged. Moreover, the γ and E 0 values plotted are unchanged yet appear on semilogarithmic scales.
Paper: Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Figure caption: The analytic procedure for TIC 11619404. Panel (a): the K95+ model (solid red line) fitted to the phase-folded light curve (black dots). Panel (b): the residuals of the fit in panel (a), and the blue dots are medians in 0.01 phase bins. Panel (c): the Fourier spectrum of the residuals from panel (b). The red and blue vertical dashed lines represent the orbital harmonics n; the blue lines indicate that they are harmonic TEOs. The solid red line shows the level of S/N = 4.0. Panel (d): the pulsation phases of the TEOs. The gray, light blue, and green strips indicate the m = 0, +2, and −2 modes, respectively. The phases of the m = +2, −2 modes are shown next to the strips. The width of the strips results from the uncertainties of T 0p  and ω. The blue circle represents a TEO with its harmonic number n; the size corresponds to its amplitude; the error bar corresponds to the uncertainty of its phase.
Paper: Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Figure caption: Same as Figure 1 for TIC 447927324.
Paper: Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Figure caption: Same as Figure 1 for TIC 266809405.
Paper: Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Figure caption: Same as Figure 1 for TIC 412881444.
Paper: Five New Heartbeat Star Systems with Tidally Excited Oscillations Discovered Based on TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Figure caption: Same as Figure 1 for TIC 266894805.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Outcomes of the long-term secular simulations. The three columns correspond to the three distinct simulation suites. In the top row, each simulation is summarized as a single dot in the space of initial inclination of the inner planet vs. its semimajor axis, with the color bar indicating the standard deviation of the inner planet’s inclination throughout the simulation. In the bottom row, the initial values of η ⋆, η GR, and 6 + η ⋆ are plotted for each simulation to give context to the simulation results. Note that η ⋆ and η GR are computed using fiducial pre-main-sequence values R ⋆ = 1.3 R ⊙ and P ⋆ = 7 days, and then these values are used to calculate the critical inclination that the inner planet is initialized with. Overall, the standard deviation is nearly zero for most runs, indicating that the inner planet’s inclination generally stays very stable.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: HAT-P-11 b evolution. These simulations show the long-term evolution of HAT-P-11 b immediately following a theorized disk-driven resonant encounter that established its polar orbit. From top to bottom, we show the evolution of planet b’s inclination, eccentricity, and semimajor axis over time. The gray lines represent the entire sample of runs. The blue lines denote the 120 runs that end with an eccentricity and semimajor axis consistent with the observed values with a tolerance of 0.05 for eccentricity and 0.005 au for semimajor axis. The polar orbit is extremely stable.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Short-term N-body simulations with and without tides. We show the early evolution of a synthetic system with representative parameters (see details in the text) as it encounters the disk-driven inclination resonance. The magenta and blue lines show the results without tides and with tides, respectively. The left panel shows the inner and outer planets’ inclinations, while the right panel shows their eccentricities. Notably, the tides-free simulation replicates the result shown in P20, thus validating our numerical method. The simulation with tides shows a similar inclination evolution, suggesting that tides do not significantly affect the near-polar outcome.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Simulation outcomes split by the amount of inclination variations. The top (bottom) panel shows the subset of simulations from all three suites where the standard deviation of the inner planet’s inclination is greater (smaller) than 1°. Notably, all polar planets are stable and only appear in the low-standard-deviation subset. Even within that subset, they are the most stable.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Tidal Q constraints. The top and bottom panels pertain to HAT-P-11 b and WASP-107 b, respectively. They show the initial eccentricity of the planet vs. its initial Q value. Each dot corresponds to a different simulation, and the coloring indicates the difference of the final eccentricity from the observed eccentricity, where red (blue) dots indicate a final eccentricity that is too high (too low). The black line represents an approximate contour overlaying the simulations with the closest match to the observed eccentricity. The empty corner in the upper right of the top panel is due to filtering out runs where the planet spirals into the star.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Parameter space for planetary obliquity excitation. The heat map indicates the initial value of ∣g ⋆,1∣/α 1 as a function of a 1 and a combination of stellar parameters. The planet is given fiducial parameters equal to m 1 = 10 M ⊕, R 1 = 3 R ⊕, k 2,1 = 0.4, and C 1 = 0.25. Obliquity excitation is expected when ∣g ⋆,1∣/α 1 > 1 for initial values. However, for the parameter space that leads to polar orbits, ∣g ⋆,1∣/α 1 ≪ 1.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Variation of the critical inclination with η ⋆ and η GR. The color bar indicates the value of the critical inclination (Equation (4)), and contours are shown in 5° increments. The white region indicates where I crit is undefined (since the argument of the arcsin is greater than 1). Such cases would reach a polar orbit without undergoing eccentricity excitation.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Example of orbital evolution for a simulation with significant inclination variation. We show the time evolution of the inner planet’s inclination, eccentricity, and semimajor axis from left to right. This simulation is the one with the most variation in the inner planet’s inclination out of all suites. The eccentricity of the inner planet rises due to interactions with the outer planet. It then undergoes rapid tidally driven eccentricity and inclination damping and inward orbital migration.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: WASP-107 b evolution. Same as Figure 8, except for WASP-107 b.
Paper: Very Extended Ionized Gas Discovered around NGC 1068 with the Circumgalactic Hα Spectrograph
Authors: Nicole Melso, David Schiminovich, Meghna Sitaram, Ignacio Cevallos-Aleman, Bárbara Cruvinel Santiago, Brian Smiley, Hwei Ru Ong
Figure caption: Top: CHαS spectral imaging of NGC 1068. The CHαS data comprise a grid of spectra; dispersed stars appear as elongated continua spectra while narrow line-width emission (e.g., bright sky lines, Hα) results in short spectra composed of only a few resolution elements. A Sloan Digital Sky Survey u-band image of the NGC 1068 galactic disk is overlaid for reference (K. N. Abazajian et al. 2009). The CHαS data presented here are not sky subtracted; the background is dominated by the bright OH 6-1P1e,1f (4.5) emission line (doublet) at 6578 Å. We label the ribbon feature (with zoom in) and other previously known structure including filament A, filament B, and the star-forming ring. Bottom: GALEX FUV (blue) and NUV (yellow) composite image with WCS applied. We label the ribbon feature (with zoom in).
Paper: Very Extended Ionized Gas Discovered around NGC 1068 with the Circumgalactic Hα Spectrograph
Authors: Nicole Melso, David Schiminovich, Meghna Sitaram, Ignacio Cevallos-Aleman, Bárbara Cruvinel Santiago, Brian Smiley, Hwei Ru Ong
Figure caption: CHαS spectral extraction and flux calibration for the ribbon. All panels have been rotated (∼15°) to align the hexagonally packed spectra along the Cartesian y-axis. The transformed coordinates can be compared directly with Figure 1. Left: flux in each spatial-spectral pixel of the sky-background-subtracted ribbon data. Middle: raw spectra extracted from each lenslet and the Gaussian fit. The spectral amplitude has been scaled to reduce overlap in this plot; however, the relative amplitude between spectra remains unchanged. Right: surface brightness in each lenslet (2.″55 diameter, 5 arcsec2 solid angle) extracted with aperture photometry. We sum the flux across each spectrum aperture, integrating over the line width, and then divide by the lenslet solid angle.