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We used the Las Cumbres Observatory telescopes to take images of three star systems: WDS 19576+3454, WDS 06043+2327, and WDS 06076+2457, on April 3rd, April 8th, and April 4th, 2024 respectively. We analyzed their astronomical measurements using Afterglow Workbench. For WDS 19576+3454, the position angle was measured to be 265.2° ± 0.12° with an angular separation of 7.38” ± 0.022”. For WDS 06043+2327, the position angle was measured to be 298.5° ± 0.28° with an angular separation of 9.83” ± 0.036”. The new data show that both WDS 19576+3454 and WDS 06043+2327 are consistent with being physical binaries but the parallax distances from the GAIA data suggest the stars in these pairs are too far apart to be gravitationally bound. Thus we conclude these two pairs are likely optical doubles. For WDS 06076+2457, the position angle was measured to be 348.1° ± 0.10° with an angular separation of 7.96” ± 0.023”. The new data we observed, combined with available GAIA data, give evidence that WDS 06076+2457 may be a physical double. 

We have taken astrometric measurements of three star systems: WDS 00033+5332 A 1500 AB,C, WDS 05283+0358 HJ 2266, and WDS 19557+3805 DAM 1 AB. We used the Las Cumbres Observatory telescopes to take images of these star systems, and we then analyzed them using Afterglow Workbench. For WDS 00033+5332, we found the position angle to be 81.62° ± 0.45° and an angular separation of 9.01’’ ± 0.04’’. Based on our analysis, we were not able to determine whether the WDS 00033+5332 double is physical. For WDS 05283+0358, we found the position angle to be 37.58° ± 0.15° and an angular separation of 7.29’’ ± 0.04’’. It is already known that WDS 05283+0358 is a physical double, and our new data supports this claim. For WDS 19557+3805, we found the position angle to be 234.64° ± 0.63° and an angular separation of 6.89’’ ± 0.10’’. Our new data points suggest this system is gravitationally bound 

This investigation selected a double star system: ES1144 (also known as HD67007A and HD67007B), which is an eclipsing binary and member of a quadruple star system. We report on our observations and measurements of position angle and separation using images taken with Las Cumbres Observatory telescopes. We found a separation of 6.7 arcsec and a position angle of 337°. We conclude that more observations will be required to establish the orbit of the system. 

We report the measurement of the position angle and separation for the double star system HD 80460. We made use of a 0.4m telescope from Las Cumbres Observatory (LCOGT) and a DeltaRho 350 + QHY600 camera. An analysis was made with the historical data from the Washington Double Star (WDS) catalog. A search was made with SIMBAD for spectral type, parallax, and proper motion for the double star. 

We report on our observations of the double star system WDS23516+0814 (CHE 506, HD 223638). We selected a double star system with a few historical observations to contribute to the determination of its possible orbit. 

Abstract We present mid-infrared spectroscopic observations of the nucleus of the nearby Seyfert galaxy NGC 7469 taken with the MIRI instrument on the James Webb Space Telescope (JWST) as part of Directors Discretionary Time Early Release Science program 1328. The high-resolution nuclear spectrum contains 19 emission lines covering a wide range of ionization. The high-ionization lines show broad, blueshifted emission reaching velocities up to 1700 km s −1 and FWHM ranging from ∼500 to 1100 km s −1 . The width of the broad emission and the broad-to-narrow line flux ratios correlate with ionization potential. The results suggest a decelerating, stratified, AGN-driven outflow emerging from the nucleus. The estimated mass outflow rate is 1–2 orders of magnitude larger than the current black hole accretion rate needed to power the AGN. Eight pure rotational H 2 emission lines are detected with intrinsic widths ranging from FWHM ∼125 to 330 km s −1 . We estimate a total mass of warm H 2 gas of ∼1.2 × 10 7 M ⊙ in the central 100 pc. The PAH features are extremely weak in the nuclear spectrum, but a 6.2 μ m PAH feature with an equivalent width of ∼0.07 μ m and a flux of 2.7 × 10 −17 W m −2 is detected. The spectrum is steeply rising in the mid-infrared, with a silicate strength of ∼0.02, significantly smaller than seen in most PG QSOs but comparable to other Seyfert 1s. These early MIRI mid-infrared IFU data highlight the power of JWST to probe the multiphase interstellar media surrounding actively accreting supermassive black holes. 

Abstract We present results from the James Webb Space Telescope Director’s Discretionary Time Early Release Science program 1328 targeting the nearby, luminous infrared galaxy, VV 114. We use the MIRI and NIRSpec instruments to obtain integral-field spectroscopy of the heavily obscured eastern nucleus (V114E) and surrounding regions. The spatially resolved, high-resolution spectra reveal the physical conditions in the gas and dust over a projected area of 2–3 kpc that includes the two brightest IR sources, the NE and SW cores. Our observations show for the first time spectroscopic evidence that the SW core hosts an active galactic nucleus as evidenced by its very low 6.2μm and 3.3μm polycyclic aromatic hydrocarbon equivalent widths (0.12 and 0.017μm, respectively) and mid- and near-IR colors. Our observations of the NE core show signs of deeply embedded star formation including absorption features due to aliphatic hydrocarbons, large quantities of amorphous silicates, as well as HCN due to cool gas along the line of sight. We detect elevated [Feii]/Pfαconsistent with extended shocks coincident with enhanced emission from warm H₂, far from the IR-bright cores and clumps. We also identify broadening and multiple kinematic components in both H₂and fine structure lines caused by outflows and previously identified tidal features.