Antiparticles

Nearly a half century after the discovery of the antiproton the study of cosmic-ray antimatter continues to be an exciting and fertile field. Sensitive searches for heavy cosmic-ray antimatter continue, although in recent years their value as a probe of universal baryon symmetry has all but evaporated. Antiprotons and positrons have opened new windows on the origin and history of cosmic rays. The rarity of antimatter as compared to ordinary cosmic-ray species has posed substantial experimental challenges. Early reports of significant enhancements of antiprotons and high-energy positrons fueled speculation that non-baryonic dark matter had been found. A new generation of balloon-borne magnetic spectrometers employing powerful particle identification techniques to eliminate background have finally managed to uncover the true antimatter signal. These new measurements support simple models of secondary production but also suggest the possibility of a small yet interesting primary component.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/43807/1/11214_2004_Article_382988.pd

Granite–a new telescope for TeV gamma ray astronomy

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87435/2/253_1.pd

Detection of TeV gamma rays from the AGN Markarian 421

We present here the detection of TeV gamma rays from the extragalactic source Markarian 421. Observations obtained with the Whipple 10 m imaging Cherenkov telescope in March–June 1992 give a gamma ray signal with statistical significance of 6.3σ above background. The excess corresponds to an average flux of 1.5×10−11 cm−2 s−1 above 0.5 TeV, equivalent to 0.3 of that from the Crab Nebula. The estimated location of the source agrees with the position of Mrk 421 to the angular uncertainty of the Whipple instrument (6 arc minutes).Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87671/2/185_1.pd

TEV gamma ray emission from the active galactic nucleus Markarian 421

TeV energy gamma ray emission from the blazar Markarian 421 was detected with the Whipple 10 meter imaging Cherenkov telescope initially during the observation period March‐June 1992 at an average photon flux of 1.5×10−11 cm2 s−1. The photon spectrum in the TeV range lies on the extrapolation of the data points observed by EGRET during viewing phase I and indicates that the emission follows an unchanged power law between 100 MeV and 10 TeV with no significant intergalactic absorption. More recent observations from the spring of 1993 confirm the 1992 measurements. Here we give an update on the status of the observations, the analysis for time variability, and the results from the analysis to determine the spectral index for Markarian 421 at TeV energies.The search for TeV emission from other extragalactic sources detected by the EGRET instrument on the Compton Gamma Ray Observatory at GeV energies have so far been negative.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87648/2/597_1.pd

Observations of the Crab nebula at TeV energies

The results of four years of observation of the Crab Nebula at TeV energies by the Whipple group are discussed and the status of the Crab Nebula as a standard candle for TeV astronomy is reviewed.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87647/2/270_1.pd

Searches for bursts of TEV gamma rays on time‐scales of seconds

The Whipple Observatory gamma‐ray telescope has a high sensitivity to sources of gamma rays in the 0.4 to 4 TeV energy range. Although this sensitivity is used primarily to search for discrete sources of gamma‐rays the instrument also has sensitivity to gamma‐ray bursts on time‐scales from milliseconds to seconds. The field of view is limited but the source location capability is good. Such bursts could radiate with peak luminosity at TeV energies and could originate from(a) primordial black holes or (b) cosmic strings; they could also be the high energy counterparts of BATSE‐type bursts and hence of unknown origin. The search of the Whipple data‐base for statistically unlikely consecutive events on time‐scales of second will be described and compared with the theoretical predictions. © 1994 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87630/2/470_1.pd

Searches for TeV counterparts to classical gamma-ray bursts

Intense effort has gone into the observation of optical, radio and X-ray GRB counterparts, either simultaneous to the burst or as quasi-steady remnants. Here we report on a similar study at higher energies of 250 GeV and above using ground-based telescopes. Imaging atmospheric Cherenkov telescopes have achieved great sensitivity and now complement observations by orbiting telescopes such as CGRO. Previous studies of bursts by the Whipple Collaboration (4) combined with recent improvements to the telescope, indicate that sensitivity to a fluence of 6×10−9 erg-cm−26×10−9erg-cm−2 can be achieved. Observations by the Whipple Collaboration of nine BATSE positions, one within 2 minutes of the BATSE burst, using coordinates distributed through BACODINE will be reported. Analysis techniques will be described and an upper limit to the high-energy delayed or extended emission of observed candidates will be calculated. © 1996 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87365/2/603_1.pd

The frequency of metal enrichment of cool helium-atmosphere white dwarfs using the DESI early data release

There is an overwhelming evidence that white dwarfs host planetary systems; revealed by the presence, disruption, and accretion of planetary bodies. A lower limit on the frequency of white dwarfs that host planetary material has been estimated to be ≃ 25–50 per cent; inferred from the ongoing or recent accretion of metals on to both hydrogen-atmosphere and warm helium-atmosphere white dwarfs. Now with the unbiased sample of white dwarfs observed by the Dark Energy Spectroscopic Instrument (DESI) survey in their Early Data Release (EDR), we have determined the frequency of metal enrichment around cool-helium atmosphere white dwarfs as 21 ± 3 per cent using a sample of 234 systems. This value is in good agreement with values determined from previous studies. With the current samples we cannot distinguish whether the frequency of planetary accretion varies with system age or host-star mass, but the DESI data release 1 will contain roughly an order of magnitude more white dwarfs than DESI EDR and will allow these parameters to be investigated

The DESI survey validation : results from visual inspection of bright galaxies, luminous red galaxies, and emission line galaxies

Funding: TWL was supported by the Ministry of Science and Technology (MOST 111-2112-M-002-015-MY3), the Ministry of Education, Taiwan (MOE Yushan Young Scholar grant NTU-110VV007), National Taiwan University research grants (NTU CC-111L894806, NTU- 111L7318), and NSF grant AST-1911140. DMA acknowledges the Science Technology and Facilities Council (STFC) for support through grant code ST/T000244/1. This research is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; additional support for DESI is provided by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technologies Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: https://www.desi.lbl.gov/ collaborating-institutions.The Dark Energy Spectroscopic Instrument (DESI) Survey has obtained a set of spectroscopic measurements of galaxies for validating the final survey design and target selections. To assist these tasks, we visually inspect (VI) DESI spectra of approximately 2,500 bright galaxies, 3,500 luminous red galaxies, and 10,000 emission line galaxies, to obtain robust redshift identifications. We then utilize the VI redshift information to characterize the performance of the DESI operation. Based on the VI catalogs, our results show that the final survey design yields samples of bright galaxies, luminous red galaxies, and emission line galaxies with purity greater than 99%. Moreover, we demonstrate that the precision of the redshift measurements is approximately 10 km/s for bright galaxies and emission line galaxies and approximately 40 km/s for luminous red galaxies. The average redshift accuracy is within 10 km/s for the three types of galaxies. The VI process also helps to improve the quality of the DESI data by identifying spurious spectral features introduced by the pipeline. Finally, we show examples of unexpected real astronomical objects, such as Lyman α emitters and strong lensing candidates, identified by VI. These results demonstrate the importance and utility of visually inspecting data from incoming and upcoming surveys, especially during their early operation phases.Publisher PDFPeer reviewe

Preliminary Target Selection for the DESI Milky Way Survey (MWS)

International audienceThe DESI Milky Way Survey (MWS) will observe $\ge$8 million stars between $16 < r < 19$ mag, supplemented by observations of brighter targets under poor observing conditions. The survey will permit an accurate determination of stellar kinematics and population gradients; characterize diffuse substructure in the thick disk and stellar halo; enable the discovery of extremely metal-poor stars and other rare stellar types; and improve constraints on the Galaxy's 3D dark matter distribution from halo star kinematics. MWS will also enable a detailed characterization of the stellar populations within 100 pc of the Sun, including a complete census of white dwarfs. The target catalog from the preliminary selection described here is public