adsabs/AstroCLIMB huggingface dataset:
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Dark matter surface density (first row), stellar surface density (second row), gas surface density (third row), density-weighted projection of gas temperature (fourth row), and density-weighted projection of gas metallicity (fifth row) through a slab of thickness 200 kpc at z = 4 in our CosmoRun simulation suite. See Appendix E.2.5 for more information on CosmoRun and this figure. Simulations performed by: Santi Roca-Fàbrega (ART-I, RAMSES), Ji-hoon Kim (ENZO), Johnny Powell and Héctor Velázquez (CHANGA), Kentaro Nagamine and Ikkoh Shimizu (GADGET-3), Kentaro Nagamine and Pablo Granizo (GADGET-4), Loic Hausammann and Yves Revaz (GEAR), Anna Genina (AREPO-T), and Alessandro Lupi and Bili Dong (GIZMO).
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Similar to Figure 27, but now with colors representing the total metal mass in each two-dimensional bin in our CosmoRun simulation suite. Note that the PDF is for the gas within Rvir from the center of the target galaxy in the CosmoRun simulations. A sphere of radius Rvir encloses the main galaxy and CGM, but not the IGM. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Stellar mass growth histories for the Cal-4 runs inside an Rvir sphere centered at the target progenitor. The curve is computed using the ages or creation times recorded in star particles at z = 4. Therefore, what we show here is an upper limit for the total M⋆ formed inside Rvir. The stellar mass range at z = 4 targeted in our calibration is M⋆ ∼ 1–5 × 109 M⊙, as motivated by semiempirical models. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: The z = 4 composite of two-dimensional PDF of density and temperature for the gas within the mean Rvir among the codes (∼25.4 kpc) from the target galaxy’s center in the CosmoRun simulations. A black dashed vertical line marks the density threshold for star formation. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Distribution of stellar mass as a function of stellar metallicity at z = 4 for all the stars inside the target progenitor’s Rvir in our CosmoRun simulation suite. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Distribution of gas mass as a function of gas metallicity at z = 4 for all the gas inside the target progenitor’s Rvir in our CosmoRun simulation suite. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Stellar mass growth histories for the Cal-3 runs in a 100 kpc sphere centered at the target progenitor. The curve is computed using the ages or creation times recorded in star particles at z = 7. See Appendix E.2.3 for more information on Cal-3 and this figure.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Spherically averaged gas density profile as a function of distance from the target progenitor’s center at z = 4 in our CosmoRun simulation suite. See Appendix E.2.5 for more information on CosmoRun and this figure.
Paper: Quasiperiodic Fast-propagating Waves Driven by the Tuning-fork Effect during Magnetic Reconnection
Authors: Jialiang Hu, Xiaozhou Zhao, Guiping Zhou, Yuhao Chen, Chunlan Jin, Leping Li, Mijie Shi, Guanchong Cheng, Xiaoxia Yu, Jing Ye, Xinping Zhou
Figure caption: Schematic diagram illustrating the generation of QFP waves. During a solar eruption, magnetic reconnection takes place within a vertical CS, propelling the erupting structure, as shown by the pink twisted topology. The vertical CS is highlighted by the thick yellow lines and exhibits two fork structures at its opposing ends. Inflow during reconnection is indicated by the bold gray arrows, while reconnection outflows are represented by two thick vertical arrows at each end. These outflows strike the termination shock structures, as indicated by the navy blue ellipses, leading to reflection. The sky blue ripple structures denote “W1” and “W2.”
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Comparison of mean stacked aperture fluxes (colored crosses) for individual fields in magnitude bins of width Δm = 0.5, field-averaged magnitudes (black), and masking catalog predictions (blue). We find close agreement between measurements and predictions across the range mAB = 17.0–19.5, with the exception of J = 17.5–18.5, in which we measure slightly higher average fluxes.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Example of data processing for CIBER 1.1 μm observations of the Boötes A field. The top left panel shows the image converted from digital units to sky brightness units and after applying the instrument mask, which removes errant pixels and regions affected by multiplexer glow. We then subtract the DC template (top middle panel). The top right panel shows the same field after DC subtraction and application of the astronomical mask. The bottom left panel shows the FF estimated from the other four fields, while the bottom middle panel shows the best-fit filtered component. Finally, the bottom right panel shows the FF-corrected, filtered, and mean-subtracted map, with rescaled color bar limits (relative to the initial map) in order to highlight residual structure after map processing.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Peak-normalized filter transmission curves for the data sets used in this work. The CIBER imagers (bold) are centered at 1.05 and 1.79 μm (third and fourth flights). We also plot the filters from Pan-STARRS (K. C. Chambers et al. 2016) in the optical and 2MASS in the NIR. In Section 8.2.2 we cross-correlate against IRAC mosaics from the SDWFS (M. L. N. Ashby et al. 2009) at 3.6 and 4.5 μm.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Example dark differences (left column) and 2D power spectra averaged over exposure pairs (right column). These match the integration time of science field elat10. Read noise is highly anisotropic in Fourier space, which we take advantage of by applying inverse-variance weighting of the measured 2D power spectrum before computing azimuthally averaged bandpowers.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Comparison of CIBER-measured source fluxes and color-corrected 2MASS fluxes, before outlier rejection is applied. The colored vertical lines indicate the minimum flux thresholds used to obtain the gain estimates in the legend. These indicate the stability of our gain solutions to the choice of minimum 2MASS flux. The quantity gag1g2 has units of (nW m−2 sr−1)/(ADU frame−1).
Paper: The Role of Magnetospheric Rebound in Breaking Resonant Chains of Super-Earths and Mini-Neptunes
Authors: Mengrui Pan, Andre Izidoro, Sho Shibata
Figure caption: Same as Figure A1 but for disks without rebound effects.
Paper: The Role of Magnetospheric Rebound in Breaking Resonant Chains of Super-Earths and Mini-Neptunes
Authors: Mengrui Pan, Andre Izidoro, Sho Shibata
Figure caption: Same as Figure A1 but for short disk lifetime cases.
Paper: The Role of Magnetospheric Rebound in Breaking Resonant Chains of Super-Earths and Mini-Neptunes
Authors: Mengrui Pan, Andre Izidoro, Sho Shibata
Figure caption: Same as Figure A1 but for long disk lifetime models.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: CIBER auto power spectrum measurements for 1.1 μm (left) and 1.8 μm (right), with Dℓ = ℓ(ℓ + 1)Cℓ/2π. The per-field measurements are shown with colored points while the weighted field averages are plotted in black. Also shown is the estimated DGL contribution (black solid lines) with shaded regions spanning 1σ and 2σ uncertainties (see Section 9). The dashed blue and solid red curves show the predicted ISL and IGL angular power spectra, described in Section 11.1. The measurements show large-angle fluctuation power exceeding that from our IGL+ISL+DGL model (dark blue curves). We do not include model-based uncertainties for IGL or ISL; however these are discussed in Section 11. Angular multipoles 100 < ℓ < 300 are technically accessible within the CIBER FOV, but are suppressed by aggressive image filtering.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: CIBER 1.1 μm (left) and 1.8 μm (right) power spectra at varying source masking depths, along with IGL+ISL model predictions (colored curves; see Section 11.1). DGL constraints are shown in black with ±1σ/2σ uncertainties (see Section 9). Here we plot ℓCℓ/2π rather than Dℓ in order to reduce the dynamic range between cases. On large angular scales (ℓ < 2000), the fluctuation power varies for the shallowest masking depths but is insensitive to source masking beyond J = 16 and H = 16.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Noise model validation for 1.1 μm (top two rows) and 1.8 μm using flight half-exposure differences. We show the power spectra of the flight differences (colored points) and those from 1000 simulated noise differences (black points). The gray solid lines indicate the photon noise contribution to the difference spectra, while the dashed lines show the point-source leakage due to pointing drift. All power spectra have been corrected for mode coupling from masking and filtering. The shaded region indicates scales at multipole ℓ > 10,000 that we do not include in the χ2 calculation. In each inset we plot the reduced χ2 distribution of noise realizations relative to the mean of the noise model, along with that of the observed data.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Sensitivity of CIBER auto power spectra to source masking radius, for 1.1 μm (top) and 1.8 μm (bottom). The first set of results come from perturbing all source radii, while the second come from perturbing only the fainter (J > 14 and H > 14) source radii. In both cases, the power spectra are consistent with the fiducial results to within uncertainties on large scales and within ±15% on scales ℓ > 10,000.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Fractional deviation of the individual field CIBER 1.1 μm power spectra relative to the weighted field average. We test consistency of the per-field auto power spectra on scales ℓ < 10,000 by computing a χ2 statistic between each field and the average, using bandpower covariances derived from an ensemble of 1000 mock recovered power spectra. In the insets, we plot the distribution of χ2 values from the mock ensemble recovered power spectra and compare against the χ2 of the observed data (colored vertical lines) to determine a PTE value for each field.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Sensitivity of CIBER auto power spectra to different assumed gain factors g1, for 1.1 μm (top) and 1.8 μm (bottom). This gain factor determines the ratio between read noise and photon noise. The recovered power spectra on scales ℓ < 30,000 are largely insensitive to changes in g1.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Same as Figure 10 but for 1.8 μm.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Cross power spectra of CIBER 1.1 and 1.8 μm exposure half-differences. These constrain the presence of any time-variable signals (over the course of one exposure) seen across imagers. We find that all cross power spectra are consistent with zero.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: CIBER pixel-convolved beam functions for both imagers. These are derived from the best-fit PSF models obtained from stacking in Y.-T. Cheng et al. (2021).
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Validation of read noise models for CIBER imagers with full-array (left set) and per-quadrant (right set) mean subtraction. Each set of results employs gradient filtering over the full arrays. The left panels of each set of plots show the mean unweighted power spectrum of exposure differences taken before flight (black) and Gaussian read noise model realizations (red). Each right subpanel in each set shows the dispersion of power spectra, normalized to ﹩\langle {N}_{\ell }^{\mathrm{model}}\rangle ﹩. We plot the noise power spectra in sky units, but without correction for the beam transfer function Bℓ.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Cross correlation coefficients of CIBER and Spitzer band combinations as a function of angular multipole. Black points indicate the field-averaged estimates from the total measured fluctuation power. The solid blue curves indicate predictions from our IGL+ISL model, which have small but nonzero variation in rℓ. For all band combinations aside from 3.6 μm × 4.5 μm, we find that fluctuations across wavelengths decorrelate going from ℓ = 10,000 to ℓ = 1000. The red points indicate the binned rℓ estimates after subtracting predicted IGL+ISL+DGL contributions from the observed power spectra.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Comparison of auto and cross power spectra using different Spitzer mosaicking algorithms. In the left panel we show Spitzer internal auto and cross power spectrum ratios, while in the right panel we show the same but for CIBER × Spitzer cross power spectra. The gray bands indicate ±5% deviations in recovered power.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Wavelength dependence of surface brightness fluctuations from CIBER and Spitzer auto power spectra, for a set of broad bandpowers spanning 875 < ℓ < 100,000. The horizontal error bars indicate the effective wavelength range spanned by the CIBER and IRAC filters. We find that the angular fluctuations on large scales are bluer than the observed and predicted Poisson fluctuations for ℓ < 4000.
Paper: CIBER Fourth-flight Fluctuation Analysis: Measurements of Near-infrared Auto and Cross Power Spectra on Arcminute to Subdegree Scales
Authors: Richard M. Feder, James J. Bock, Yun-Ting Cheng, Asantha Cooray, Phillip M. Korngut, Shuji Matsuura, Jordan Mirocha, Chi H. Nguyen, Kohji Takimoto, Kohji Tsumura, Ryan Wills, Michael Zemcov
Figure caption: Correlation of CIBER 1.1 μm (blue), 1.8 μm (red), and 1.1 μm × 1.8 μm (purple) power spectrum bandpowers with respect to ZL intensity from T. Kelsall et al. (1998) (top panels) and DGL intensity (bottom). The lack of correlation rules out the presence of additional foreground fluctuations that are correlated with ZL and DGL but are not captured by existing tracer maps/models.