es/iode’s Post

📃Scientific paper: Millimeter-wave CO and SiO Observations toward the Broad-velocity-width Molecular Feature CO 16.134-0.553: a Smith cloud scenario? Abstract: We report the results of the CO $\textit J$=1-0 and SiO $\textit J$=2-1 mapping observations towards the broad-velocity-width molecular feature CO 16.134-0.553 with the Nobeyama Radio Observatory 45 m telescope. The high quality CO map shows that the 5-pc size broad-velocity-width feature bridges two separate velocity components at $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ and 65 km s$^\{-1\}$ in the position-velocity space. The kinetic power of CO 16.134-0.553 amounts to $7.8\times10^2$ $\textit L$$\_\odot$ whereas no apparent driving sources were identified. Prominent SiO emission was detected from the broad-velocity-width feature and its root in the $\textit V\_\{\rm\{LSR\}\}$$\quad$$\simeq$ 40 km s$^\{-1\}$ component. In the CO Galactic plane survey data, CO 16.134-0.553 appears to correspond to the Galactic eastern rim of a 15-pc diameter expanding CO shell. An $1\deg$-diameter H I emission void and $4\deg$-long vertical H I filament were also found above and below the CO shell, respectively. We propose that the high-velocity plunge of a dark matter subhalo with a clump of baryonic matter was responsible for the formation of the H I void, CO 16.134-0.553/CO shell, and the H I filament. ;Comment: 7 pages, 6 figures, 2 table, accepted for publication in ApJ Continued on ES/IODE ➡️ https://etcse.fr/Bmuf ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: The FAST all sky HI survey (FASHI): The first release of catalog Abstract: The FAST All Sky HI survey (FASHI) was designed to cover the entire sky observable by the Five-hundred-meter Aperture Spherical radio Telescope (FAST), spanning approximately 22000 square degrees of declination between -14 deg and +66 deg, and in the frequency range of 1050-1450 MHz, with the expectation of eventually detecting more than 100000 HI sources. Between August 2020 and June 2023, FASHI had covered more than 7600 square degrees, which is approximately 35% of the total sky observable by FAST. It has a median detection sensitivity of around 0.76 mJy/beam and a spectral line velocity resolution of ~6.4 km/s at a frequency of ~1.4 GHz. As of now, a total of 41741 extragalactic HI sources have been detected in the frequency range 1305.5-1419.5 MHz, corresponding to a redshift limit of z<0.09. By cross-matching FASHI sources with the Siena Galaxy Atlas (SGA) and the Sloan Digital Sky Survey (SDSS) catalogs, we found that 16972 (40.7%) sources have spectroscopic redshifts and 10975 (26.3%) sources have only photometric redshifts. Most of the remaining 13794 (33.0%) HI sources are located in the direction of the Galactic plane, making their optical counterparts difficult to identify due to high extinction or high contamination of Galactic stellar sources. Based on current survey results, the FASHI survey is an unprecedented blind extragalactic HI survey. It has higher spectral and spatial resolution and broader coverage than the Arecibo Legacy Fast ALFA Survey (ALF... Continued on ES/IODE ➡️ https://etcse.fr/iGKHn ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: The FAST all sky HI survey (FASHI): The first release of catalog Abstract: The FAST All Sky HI survey (FASHI) was designed to cover the entire sky observable by the Five-hundred-meter Aperture Spherical radio Telescope (FAST), spanning approximately 22000 square degrees of declination between -14 deg and +66 deg, and in the frequency range of 1050-1450 MHz, with the expectation of eventually detecting more than 100000 HI sources. Between August 2020 and June 2023, FASHI had covered more than 7600 square degrees, which is approximately 35% of the total sky observable by FAST. It has a median detection sensitivity of around 0.76 mJy/beam and a spectral line velocity resolution of ~6.4 km/s at a frequency of ~1.4 GHz. As of now, a total of 41741 extragalactic HI sources have been detected in the frequency range 1305.5-1419.5 MHz, corresponding to a redshift limit of z<0.09. By cross-matching FASHI sources with the Siena Galaxy Atlas (SGA) and the Sloan Digital Sky Survey (SDSS) catalogs, we found that 16972 (40.7%) sources have spectroscopic redshifts and 10975 (26.3%) sources have only photometric redshifts. Most of the remaining 13794 (33.0%) HI sources are located in the direction of the Galactic plane, making their optical counterparts difficult to identify due to high extinction or high contamination of Galactic stellar sources. Based on current survey results, the FASHI survey is an unprecedented blind extragalactic HI survey. It has higher spectral and spatial resolution and broader coverage than the Arecibo Legacy Fast ALFA Survey (ALF... Continued on ES/IODE ➡️ https://etcse.fr/iGKHn ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: Performance study update of observations in divergent mode for the Cherenkov Telescope Array Abstract: Due to the limited field of view (FoV) of Cherenkov telescopes, the time needed to achieve target sensitivity for surveys of the extragalactic and Galactic sky is large. To optimize the time spent to perform such surveys, a so-called "divergent mode" of the Cherenkov Telescope Array Observatory (CTAO) was proposed as an alternative observation strategy to the traditional parallel pointing. In the divergent mode, each telescope points to a position in the sky that is slightly offset, in the outward direction, from the original center of the field of view. This bring the advantage of increasing the total instantaneous arrays' FoV. From an enlarged field of view also benefits the search for very-high-energy transient sources, making it possible to cover large sky regions in follow-up observations, or to quickly cover the probability sky map in case of Gamma Ray Bursts (GRB), Gravitational Waves (GW), and other transient events. In this contribution, we present the proposed implementation of the divergent pointing mode and its first preliminary performance estimation for the southern CTAO array. ;Comment: Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219) Continued on ES/IODE ➡️ https://etcse.fr/Ped ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: Revisiting Gamma-Ray Emission of the Supernova Remnant RCW 103 Abstract: We analyze more than 15 years of the \gr\ data, obtained with the Large Area Telescope \(LAT\) onboard \{\it the Fermi Gamma-ray Space Telescope \(Fermi\)\}, for the region of the young supernova remnant \(SNR\) RCW\~103, since the nearby source 4FGL J1616.2$-$5054e, counterpart to HESS\~J1616$-$518 and $\simeq$13\,arcmin away from the SNR, is determined to be extended in the more recent Fermi-LAT source catalog. Different templates for 4FGL J1616.2$-$5054e and RCW\~103 are tested, and we find that a point source with a power-law \(PL\) spectrum at the southern limb of the SNR best describes the detected gamma-ray emission. The photon index of the PL emission is $\Gamma\simeq 2.31$\(or $\alpha\simeq 2.4$ in a Log-Parabola model\) , softer than the previously reported $\Gamma\simeq 2.0$ when the counterpart to HESS\~J1616$-$518 was considered to be a point source \(which likely caused mis-identification of extended emission at RCW\~103\). In order to produce the \gr\ emission in a hadronic scenario, we estimate that protons with an index$\sim$2.4 PL energy distribution are needed. These results fit with those from multi-wavelength observations that have indicated the remnant at the southern limb is interacting with a molecular cloud. ;Comment: 7 pages, 4 figures, 2 tables, accepted for publication in ApJ Continued on ES/IODE ➡️ https://etcse.fr/tNySC ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: A Millisecond Pulsar Binary Embedded in a Galactic Center Radio Filament Abstract: The Galactic Center is host to a population of extraordinary radio filaments, thin linear structures that trace out magnetic field lines running perpendicular to the Galactic plane. Using Murriyang, the 64 m Parkes radio telescope, we conducted a search for pulsars centered on the position of a compact source in the filament G359.0$-$0.2. We discovered a millisecond pulsar \(MSP\), PSR J1744$-$2946, with a period $P = 8.4$ ms, that is bound in a 4.8 hr circular orbit around a $M\_\{\rm c\} \> 0.05\,M\_\{\odot\}$ companion. The pulsar dispersion measure of $673.7 \pm 0.1$ pc cm$^\{-3\}$ and Faraday rotation measure of $3011 \pm 3$ rad m$^\{-2\}$ are the largest of any known MSP. Its radio pulses are moderately scattered due to multi-path propagation through the interstellar medium, with a scattering timescale of $0.87 \pm 0.08$ ms at 2.6 GHz. Using MeerKAT, we localized the pulsar to a point source embedded in a low-luminosity radio filament, the "Sunfish", that is unrelated to G359.0$-$0.2. Our discovery of the first MSP within 1$^\{\circ\}$ of the Galactic Center hints at a large population of these objects detectable via high frequency surveys. The association with a filament points to pulsars as the energy source responsible for illuminating the Galactic Center radio filaments. ;Comment: 6 pages, 4 figures, 1 table. Accepted for publication in ApJ Letters Continued on ES/IODE ➡️ https://etcse.fr/vVZ2X ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

📃Scientific paper: High-Resolution, Mid-Infrared Color Temperature Mapping of the Central 10 Arcseconds of the Galaxy Abstract: The neighborhood of the Galactic black hole boasts a plethora of extended interstellar gas and dust features as well as populations of compact \(unresolved, or marginally resolved\) features such as the G objects. Most are well manifested in the infrared. To disentangle and characterize the infrared structure of extended features and identify compact sources, we used 3.8\~$\mu$m \(L' filter\) data from the NIRC2 imager at the Keck Observatory and 8.6\~$\mu$m \(PAH1 filter\) data from the VISIR imager at the Very Large Telescope \(VLT\) to produce the highest-resolution mid-IR color-temperature map of the inner half-parsec of the Galactic Center to date. From this map, we compile a catalog of features that stand out from their background. In particular, we identify 33 compact sources that stand out against the local background temperature, 11 of which are newly identified and are candidates for being members of the G objects population. Additionally, we resolve and newly characterize the morphology of several known extended features. These results prepare the way for ongoing and future JWST studies that have access to a greater range of mid-infrared wavelengths, and thus will allow for refined estimation of the trends of dust temperatures. ;Comment: 22 pages, 14 figures Continued on ES/IODE ➡️ https://etcse.fr/40TFY ------- If you find this interesting, feel free to follow, comment and share. We need your help to enhance our visibility, so that our platform continues to serve you.

maxon Motors for Telescopes The HETDEX project (Hobby-Eberly Telescope Dark Energy Experiment) is the first major attempt to find and examine “dark energy” in the universe. Through this project, we are able to record three-dimensional positions of one million galaxies using special spectrographs. In the summer of 2012, the Hobby-Eberly Telescope began scanning the universe with the help of maxon motors for telescopes. Hobby-Eberly Telescope (HET) The Hoby-Eberly Telescope is located at the McDonald Observatory in West Texas and contains a spherical mirror with 91 identical hexagonal segments, each one meter in size. These mirror segments for a mirror with a diameter of 11 meters, making it the largest in the world. The HET in and of itself is the fourth largest optical telescope in the world, but due to its innovative design, it was cost-effective to make. Costing around $13.5 million, the HET cost about ¼ the cost of a comparably large telescope. This spectroscopic telescope is mounted on a Prime Focus Instrument Package (PFIP) equipped with two spectrographs. The mirror always points at a position 55 degrees above the horizon, but it can be swiveled horizontally full circle, allowing it to observe 70% of the skies. In future projects, upgrades to the wide field components will increase the angle of view to 22 arc minutes and usable aperture to 10 meters, making it possible to gather the highest possible light quantity via glass fiber coupling. These upgrades will revolutionize spectroscopic observation. Scientists want to use this upgraded version of the HET to obtain a better understanding of “dark energy.” Current hypotheses stipulate that almost ¾ of all matter and energy in the universe consists of “dark energy.” Dark energy is considered to be a mysterious force that causes the universe to drift apart at increasing speeds at it ages. Click below to read the complete article: https://lnkd.in/dCP4pGB9 #maxonmotor #BLDCmotor #brushlessdirectcurrentmotor

🛰️🌞 Aditya-L1 has reached its destination, the Halo orbit, showcasing ISRO's capabilities in complex orbital manoeuvres. More details: https://lnkd.in/ggpxc2gz Here's what we need to know about 🛰️Aditya-L1: 🎯 What is Aditya-L1? 📖 The India's first observatory class satellite dedicated to the comprehensive study of solar activities and its effect on space weather. It is placed around Lagrangian point 1 (L1) of the Sun-Earth system (around 1.5 million Kilometres from Earth, in a Halo orbit) 🎯 What is L1 point? 📖 For a two body gravitational system, Lagrangian points are the positions in space where a small object tends to stay, if put there. (Technically, the gravitational pull of the two bodies equals the necessary centripetal force required for a small object to move with them). There are a total of 5 Lagrangian points, L1, L2, L3, L4 and L5. Lagrangian point L1 lies between the Sun-Earth line. 🎯 Why L1? 📖 The major advantage is that sun can be continuously viewed without any occultation/eclipse. Moreover, fuel consumption is reduced as the spacecraft is relatively stationary at L1. 🎯 What are the mission objectives? 📖 The scientific objectives include the study of Coronal heating, Solar wind acceleration, Coronal Mass injections (CME), Dynamics of solar atmosphere and Temperature anisotropy. 🎯 What are the Scientific instruments onboard Aditya-L1 to achieve the mission objectives ? 📖 The 7 scientific payloads on-board Aditya-L1 include: 1. VELC (Visible Emission Line Coronagraph): ☀️ Studies the solar corona and Coronal Mass Ejections - Developed at IIA, Bengaluru 2. SUIT (Solar Ultra-violet Imaging Telescope): ☀️ Images the Solar photosphere and Chromosphere as well as measures the solar irradiance variations in near UV. - Developed at IUCAA, Pune 3. ASPEX (Aditya Solar wind Particle Experiment): ☀️ Studies the solar wind and energetic ions, as well as their energy distribution. It consists of two subsystems: a) SWIS (Solar Wind Ion Spectrometer)- 🔆 A low energy spectrometer to measure protons and alpha particles of the solar wind. b) STEPS (Suprathermal and Energetic Particle Spectrometer)- 🔆 A high energy spectrometer to measure high energy ions of the solar wind. - Developed at PRL, Ahmedabad 4. PAPA (Plasma Analyser Package for Aditya): ☀️ Studies the solar wind and its composition and does mass analysis of solar wind ions. - Developed at VSSC 5. SoLEXS (Solar Low Energy X-ray Spectrometer): ☀️ Soft X-ray Spectrometer to measure the solar soft X-ray reflux to study the solar flares. - Developed at URSC 6. HEL1OS (High Energy L1 Orbiting X-ray Spectrometer): ☀️ Hard X-ray Spectrometer to study solar flares in the high energy X-rays. - Developed at URSC 7. Magnetometer payload: ☀️ Measures the interplanetary magnetic fields at the L1 point. - Developed at LEOS 🎯 More details on the payloads: https://lnkd.in/gWTMPCiB 🚀 Mission details: https://lnkd.in/g394wN8M #Aditya-L1 #isro

Ultraviolet “winds” from nearby massive stars are stripping the gas from a young star’s protoplanetary disk, causing it to rapidly lose mass, according to a new study. It reports the first directly observed evidence of far-ultraviolet (FUV)-driven photoevaporation of a protoplanetary disk. The findings, which use observations from the James Web Space Telescope (JWST), provide new insights into the constraints of gas giant planet formation, including in our own Solar System. Young low-mass stars are often surrounded by relatively short-lived protoplanetary disks of dust and gas, which provide the raw materials from which planets form. As such, gas giant planet formation is limited by processes that remove mass from protoplanetary disks, such as photoevaporation. Photoevaporation occurs when the upper layers of protoplanetary disks are heated by x-ray or ultraviolet protons, which increases the gas temperature and causes it to escape from the system. Since most low-mass stars form in clusters also containing massive stars, protoplanetary disks are expected to be exposed to external radiation and experience ultraviolet-driven photoevaporation. Using near-infrared and submillimeter measurements from the JWST and the Atacama Large Millimeter Array (ALMA), respectively, Olivier Berné and colleagues report observations of a FUV-irradiated protoplanetary disk, d203-506, located inside the Orion Nebula. By modeling the kinematics and excitation of the emission lines detected within the PDR, the researchers found that d203-506 is losing mass at a high rate due to FUV-driven heating and ionization. #cosmos #photoevaporation #jwst #measurements https://lnkd.in/gbbuFyD8