scholarly journals Program and Results of Investigations Rapid Variability of the BL Lac Object 3C 371 in Radio and Optical Ranges

Galaxies ◽  
2020 ◽  
Vol 8 (3) ◽  
pp. 69
Author(s):  
Artem Sukharev ◽  
Michail Ryabov ◽  
Vladislavs Bezrukovs ◽  
Arturs Orbidans ◽  
Marcis Bleiders ◽  
...  
Keyword(s):  
Optical Observations ◽  
Optical Range ◽  
Owens Valley ◽  
Rapid Variability ◽  
Radio Observatory ◽  
Radio Range ◽  
Bl Lac ◽  
Cyclical Variability ◽  
Low Amplitude

BL Lac object 3C 371 is variable in optical and radio range, according to long-term monitoring data, for example AAVSO (American Association of Variable Star Observers) and OVRO (Owens Valley Radio Observatory). In addition, some authors note intra-night variability. However, in terms of access, just a few works are devoted to this topic, and questions remain about intra-day variability in radio range. The purpose of the work is to search for fast variability in radio (5, 6.1, 6.7 GHz) and optical bands (V, R, I) using international cooperation in 2019 and 2020 observation sessions. The 16-m radio telescope VIRAC, in Latvia, as well as optical telescopes AZT-3 (Mayaki, Ukraine), VNT (Vihorlat, Slovakia), and Schmidt camera (Baldone, Latvia) were used. To analyze variability, the STFT method of spectrograms and Lomb–Scargle periodograms for non-uniform time series were used. As result of the work, there is no correlation between optical and radio observations, and no significant quasi-harmonic variability was detected in radio range, but there is irregular low amplitude variability. In the optical range, there is variability with a characteristic time of about seven days and possibly less. Cyclical variability of 3C 371 was found in the optical range, and intra-day variability in radio range is most likely absent, as there are irregular variations and noise. It is planned to continue joint radio-optical observations 3C 371 to accumulate the necessary statistics.

scholarly journals Unvealing the physics of the most active of galaxies

2017 ◽  
Author(s):  
Ιωάννης Λιοδάκης
Keyword(s):  
Owens Valley ◽  
Radio Observatory ◽  
Bl Lac

Οι φλογαστέρες (blazars) είναι από τους πιο ενεργούς γαλαξιακούς πυρήνες (AGN), με σχετικιστικούς πίδακες προσανατολισμένους στο πεδίο της όρασης μας. Εξαιτίας αυτού του προσανατολισμού όλες οι παρατηρούμενες ποσότητες στρεβλώνονται λόγω σχετικιστικών διορθώσεων δημιουργώντας μοναδικά φαινόμενα όπως ενισχυμένη εκπομπή σε όλο το ηλεκτρομαγνητικό φάσμα, γρήγορη μεταβλητότητα, και φαινομενικά υπερφωτή κίνηση του πίδακα. Μικρές διαφοροποιήσεις στην γωνία θέασης, ή/και στην ταχύτητα του πίδακα μπορεί να έχει ως αποτέλεσμα μεγάλη διαφοροποίηση στις παρατηρούμενες ποσότητες από σχετικά όμοιες πηγές. Περιπλέκοντας έτσι την κατανόηση μας για τις πραγματικές τους ιδιότητες και τις διεργασίες σχετικές με τις κεντρικές μηχανές τους. Ως αποτέλεσμα, παρά τις δεκαετίες συστηματικής έρευνας πάνω στην μεταβλητότητα τους σε όλο το ηλεκτρομαγνητικό φάσμα, γνωρίζουμε ελάχιστα για τις ιδιότητες των φλογαστέρων στο σύστημα ηρεμίας του πίδακα. Για αυτούς τους λόγους, οι διατριβή μου εστίασε στον να καταλάβουμε και να ποσοτικοποιήσουμε τα σχετικιστικά φαινόμενα που κατακυριεύουν στην εκπομπή των φλογαστέρων.Δουλεύοντας προς αυτήν την κατεύθυνση, δημιούργησα πληθυσμιακά μοντέλα βασισμένα σε εύρωστες παρατηρούμενες ποσότητες ανεπηρέαστες από την μεταβλητότητα τα οποία περιγράφουν και τα BL Lac αντικείμενα και τους FSRQs. Χρησιμοποιώντας αυτά τα μοντέλα, κατάφερα προωθήσω την κατανόηση μας για τις φυσικές ιδιότητες των φλογαστέρων με τους εξής τρόπους: α) η μέθοδος της μεταβλητότητας και η μέθοδος του αντίστροφου σκεδασμού Compton για τον υπολογισμό του σχετικιστικού παράγοντα Doppler είναι οι καλύτερες διαθέσιμές μέθοδοι για να υπολογίσουμε παρατηρησιακά τους παράγοντες Doppler σε φλογαστέρες που δείχνει ότι κατά την διάρκεια εκλάμψεων οι φλογαστέρες φτάνουν σε κατάσταση "equipartition"'; β) Ενα σημαντικό μέρος των αντι-πιδάκων θα ανιχνευτούν από τα επομενής γενιάς συμβολόμετρα; γ) η εγγενή κατανομή χρόνων οποιουδήποτε τύπου γεγονότος παρόν σε φλογαστέρες μπορεί να ανακτηθεί με ακρίβεια σε στατιστικά δείγματα " flux-limited" ακόμα και αν δεν έχουμε γνώση για τις σχετικιστικές διορθώσεις για κάθε πηγή. Εφάρμοσα τα ευρήματα μου σε παρατηρήσεις φλογαστέρων: F-GAMMA: Χρησιμοποιώντας τις ραδιοφωνικές χρονοσειρές πολλαπλών μηκών κύματος του προγράμματος F-GAMMA, εκτίμησα τον παράγοντα Doppler με την μέθοδο της μεταβλητότητας για 58 πήγες με ισχυρή εκπομπή στις ακτίνες γ με κατά μέσον όρο 16% αβεβαιότητα, κάνοντας τους τους πιο ακριβής παράγοντες Doppler διαθέσιμους σήμερα. Χρησιμοποιώντας αυτούς του παράγοντες Doppler ανακάλυψα μια δυνατή συσχέτιση μεταξύ τις εγγενής βολομετρικής ραδιοφωνικής λαμπρότητας από 2.6-142.33 GHz και την μάζα της μελανής οπής που εκτείνεται εννέα τάξεις μεγέθους από αστρικής μάζας μέχρι τις πιο μαζικές μελανές οπές στο σύμπαν. Η συσχέτιση αυτή, είναι η πρώτη που ενώνει το σύστημα αναφοράς του παρατηρητή με το σύστημα ηρεμίας του πίδακα σε σχετικιστικά ενισχυόμενες πηγές.RoboPol: Ανέκτησα της εγγενή κατανομή χρόνων των μακρύτερων (σε διάρκεια) στροφών του πεδίου της πόλωσης του συμβαίνει στους φλογαστέρες. Βρήκα ότι η πιθανότερη μορφή αυτής της κατανομής είναι μια στενή κατανομή Gauss. \OVRO: Μοντελοποιώντας την κατανομή της πυκνότητας ροής των πηγών που παρατηρούνται από το 40 μέτρων ράδιοτηλεσκόπιο του Owens Valley Radio Observatory, βρήκα ότι οι πηγές με εκπομπή ακτίνων γ είναι συστηματικά πιο μεταβλητές από αυτές χωρίς εκπομπή ακτίνων γ γεγονός που υποδηλώνει την συσχέτιση μεταξύ της μεταβλητότητας στα ραδιοκύματα και την εκπομπή ακτίνων γ. Συμφιλιώνοντας τις εκτιμήσεις παραγόντων Doppler:Χρησιμοποιώντας αρχειακές παρατηρήσεις ακτίνων Χ και ραδιοφωνικής συμβολομετρίας VLBI ξανα-υπολόγισα τον παράγοντα Doppler με την μέθοδο του αντίστροφου σκεδασμού Compton για 11 πηγες με εκπομπή ακτίνων γ λαμβάνοντας υπόψιν όλες τις γνωστές πηγές σφαλμάτων τις μεθόδου. Συγκρίνοντας τις ξανα-υπολογισμένες τιμές με αυτές από την βιβλιογραφία κατάφερα να εκτιμήσω με σιγουριά τον σχετικιστικό παράγοντα Doppler για πέντε πηγές, και συγκεκριμένα τις 3C273, 3C345$, 3C454.3, PKS1510-089, και PKS1633+382.

scholarly journals 21-cm Absorption in BL Lac

1972 ◽  
Vol 44 ◽  
pp. 271-271
Author(s):  
M. H. Cohen
Keyword(s):  
Absorption Line ◽  
Optical Depth ◽  
Hydrogen Absorption ◽  
Galactic Latitude ◽  
Owens Valley ◽  
Radio Observatory ◽  
Extragalactic Object ◽  
Rotation Measure ◽  
Bl Lac ◽  
Distance Limit

Observations with the Owens Valley Radio Observatory interferometer show that BL Lac has a 21-cm hydrogen absorption line, produced by a local intervening cloud. The line is centered on zero velocity (LSR), has a width of about 5 km s−1, and shows an optical depth of 0.5. BL Lac is at galactic latitude b= −10°. No firm distance limit is possible, but such clouds are, typically, 100 pc apart. This observation is consistent with BL Lac being an extragalactic object. Other observations leading to a similar conclusion are of rotation measure (MacLeod and Andrew, 1968) and of reddening (Bertaud et al., 1969).

scholarly journals Serendipitous VLBI Observations of Intraday Variability in the BL Lac Objects 1334–127, 2131–021, and 2155–152

1998 ◽  
Vol 164 ◽  
pp. 273-274
Author(s):  
P. Yu. Kochanev ◽  
D. C. Gabuzda
Keyword(s):  
Rapid Variability ◽  
Bl Lac Objects ◽  
Polarization Structure ◽  
Vlbi Observations ◽  
Bl Lac ◽  
Vlbi Data ◽  
Intraday Variability

AbstractGlobal λ = 6 cm VLBI polarization observations of intraday variability in the three BLLacertae objects 1334–127, 2131–021, and 2155–152 are analyzed. Integrated VLA measurements during the VLBI observations show that although there were no substantial total intensity variations, the polarizations for these three sources varied significantly during the VLBI experiment. The VLBI data were divided into 2-3 hour segments in order to search for corresponding rapid variability in the VLBI polarization structure. Our analysis shows that the VLA polarization variability in 2155–152 and 2131–021 is present in the VLBI data (i.e., it occurred on mas scales), but this is not the case for 1334–127.

scholarly journals Characterizing the γ-ray long-term variability of PKS 2155−304 with H.E.S.S. and Fermi-LAT

2017 ◽  
Vol 598 ◽  
pp. A39 ◽  
Author(s):  
◽  
H. Abdalla ◽  
A. Abramowski ◽  
F. Aharonian ◽  
F. Ait Benkhali ◽  
...  
Keyword(s):  
Flicker Noise ◽  
High Energy ◽  
Long Term Results ◽  
Noise Power ◽  
Quiescent State ◽  
Physical Processes ◽  
Bl Lac Objects ◽  
Power Spectral ◽  
Bl Lac

Studying the temporal variability of BL Lac objects at the highest energies provides unique insights into the extreme physical processes occurring in relativistic jets and in the vicinity of super-massive black holes. To this end, the long-term variability of the BL Lac object PKS 2155−304 is analyzed in the high (HE, 100 MeV < E < 300 GeV) and very high energy (VHE, E > 200 GeV) γ-ray domain. Over the course of ~9 yr of H.E.S.S. observations the VHE light curve in the quiescent state is consistent with a log-normal behavior. The VHE variability in this state is well described by flicker noise (power-spectral-density index βVHE = 1.10+0.10-0.13) on timescales larger than one day. An analysis of ~5.5 yr of HE Fermi-LAT data gives consistent results (βHE = 1.20+0.21-0.23, on timescales larger than 10 days) compatible with the VHE findings. The HE and VHE power spectral densities show a scale invariance across the probed time ranges. A direct linear correlation between the VHE and HE fluxes could neither be excluded nor firmly established. These long-term-variability properties are discussed and compared to the red noise behavior (β ~ 2) seen on shorter timescales during VHE-flaring states. The difference in power spectral noise behavior at VHE energies during quiescent and flaring states provides evidence that these states are influenced by different physical processes, while the compatibility of the HE and VHE long-term results is suggestive of a common physical link as it might be introduced by an underlying jet-disk connection.

scholarly journals Explaining the trends and variability in the United States tornado records using climate teleconnections and shifts in observational practices

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Niloufar Nouri ◽  
Naresh Devineni ◽  
Valerie Were ◽  
Reza Khanbilvardi
Keyword(s):  
Population Density ◽  
Large Scale ◽  
Southern Oscillation ◽  
The United States ◽  
Anthropogenic Factors ◽  
Climate Variables ◽  
Term Trend ◽  
Cyclical Variability ◽  
Long Term Trend

AbstractThe annual frequency of tornadoes during 1950–2018 across the major tornado-impacted states were examined and modeled using anthropogenic and large-scale climate covariates in a hierarchical Bayesian inference framework. Anthropogenic factors include increases in population density and better detection systems since the mid-1990s. Large-scale climate variables include El Niño Southern Oscillation (ENSO), Southern Oscillation Index (SOI), North Atlantic Oscillation (NAO), Pacific Decadal Oscillation (PDO), Arctic Oscillation (AO), and Atlantic Multi-decadal Oscillation (AMO). The model provides a robust way of estimating the response coefficients by considering pooling of information across groups of states that belong to Tornado Alley, Dixie Alley, and Other States, thereby reducing their uncertainty. The influence of the anthropogenic factors and the large-scale climate variables are modeled in a nested framework to unravel secular trend from cyclical variability. Population density explains the long-term trend in Dixie Alley. The step-increase induced due to the installation of the Doppler Radar systems explains the long-term trend in Tornado Alley. NAO and the interplay between NAO and ENSO explained the interannual to multi-decadal variability in Tornado Alley. PDO and AMO are also contributing to this multi-time scale variability. SOI and AO explain the cyclical variability in Dixie Alley. This improved understanding of the variability and trends in tornadoes should be of immense value to public planners, businesses, and insurance-based risk management agencies.

scholarly journals Astrometric and Photometric Variability in Quasars

2009 ◽  
Vol 5 (S267) ◽  
pp. 103-103
Author(s):  
A. H. Andrei ◽  
S. Bouquillon ◽  
J. L. Penna ◽  
F. Taris ◽  
S. Anton ◽  
...  
Keyword(s):  
Strong Support ◽  
Optical Emission ◽  
Optical Observations ◽  
Massive Black Hole ◽  
Full Account ◽  
Photometric Variability ◽  
Central Engine ◽  
Relationship Of ◽  
The Relationship

Quasars are the choicest objects to define a quasi-inertial reference frame. At the same time, they are active galactic nuclei powered by a massive black hole. As the astrometric precision of ground-based optical observations approaches the limit set by the forthcoming GAIA mission, astrometric stability can be investigated. Though the optical emission from the core region usually exceeds the other components by a factor of a hundred, the variability of those components must surely imply some measure of variability of the astrometric baricenter. Whether this is confirmed or not, it puts important constraints on the relationship of the quasar's central engine to the surrounding distribution of matter. To investigate the correlation between long-term optical variability and what is dubbed as the “random walk” of the astrometric center, a program is being pursued at the WFI/ESO 2.2m. The sample was selected from quasars known to undergo large-amplitude and long-term optical variations (Smith et al. 1993; Teerikorpi 2000). The observations are typically made every two months. The treatment is differential, comparing the quasar position and brightness against a sample of selected stars for which the average relative distances and magnitudes remain constant. The provisional results for four objects bring strong support to the hypothesis of a relationship between astrometric and photometric variability. A full account is provided by Andrei et al. (2009).

VERITAS OBSERVATIONS OF RELATIVISTIC OUTFLOWS IN LOW- AND INTERMEDIATE-FREQUENCY-PEAKED BL LAC OBJECTS

2014 ◽  
Vol 28 ◽  
pp. 1460178
Author(s):  
◽  
HEIKE PROKOPH
Keyword(s):  
Gamma Ray ◽  
Intermediate Frequency ◽  
Bl Lac Objects ◽  
Bl Lacertae ◽  
Bl Lac ◽  
Bl Lacs ◽  
Gamma Ray Telescopes ◽  
Very High

The majority of blazars detected at very high energies (VHE; E > 100 GeV) are high-frequency-peaked BL Lac objects (HBLs). Low- and intermediate-frequency-peaked BL Lacs (LBLs/IBLs with synchrotron-peak frequencies in the infrared and optical regime) are generally more powerful, more luminous, and have a richer jet environment than HBLs. However, only a handful of these IBL and LBLs have been detected by ground-based gamma-ray telescopes, typically during high-flux states. The VERITAS array has been monitoring five known VHE LBLs/IBLs since 2009: 3C 66A, W Comae, PKS 1424+240, S5 0716+714 and BL Lacertae, with typical exposures of 5-10 hours per year. The results of these long-term observations are presented, including a bright, subhour-scale VHE flare of BL Lacertae in June 2011, the first low-state detections of 3C 66A and W Comae, and the detection and characterization of the IBL B2 1215+30.

Electrical Resistive Spiking of Fungi

2021 ◽  
pp. 1-7 ◽  
Author(s):  
Andrew Adamatzky ◽  
Alessandro Chiolerio ◽  
Georgios Sirakoulis
Keyword(s):  
Electrical Resistance ◽  
Electronic Devices ◽  
Low Frequency ◽  
High Amplitude ◽  
Average Amplitude ◽  
Average Width ◽  
C 23 ◽  
C 30 ◽  
Low Amplitude

We study long-term electrical resistance dynamics in mycelium and fruit bodies of oyster fungi P. ostreatus. A nearly homogeneous sheet of mycelium on the surface of a growth substrate exhibits trains of resistance spikes. The average width of spikes is c. 23[Formula: see text]min and the average amplitude is c. 1[Formula: see text]k[Formula: see text]. The distance between neighboring spikes in a train of spikes is c. 30[Formula: see text]min. Typically, there are 4–6 spikes in a train of spikes. Two types of electrical resistance spikes trains are found in fruit bodies: low frequency and high amplitude (28[Formula: see text]min spike width, 1.6[Formula: see text]k[Formula: see text] amplitude, 57[Formula: see text]min distance between spikes) and high frequency and low amplitude (10[Formula: see text]min width, 0.6[Formula: see text]k[Formula: see text] amplitude, 44[Formula: see text]min distance between spikes). The findings could be applied in monitoring of physiological states of fungi and future development of living electronic devices and sensors.

scholarly journals VLBI Measurements of Radio Source Positions at Three U.S. Stations

1981 ◽  
Vol 63 ◽  
pp. 329-336
Author(s):  
Shu-Hua Ye
Keyword(s):  
Radio Source ◽  
Radio Astronomy ◽  
Data Reduction ◽  
Geodetic Survey ◽  
Time Span ◽  
National Geodetic Survey ◽  
Owens Valley ◽  
Radio Observatory ◽  
The U.S

AbstractResults of VLBI measurement of 14 radio source positions at three U.S. stations during the MERIT short campaign is presented. Comparisons with other solutions are given, together with the comparisons between several radio source catalogues.During the MERIT short campaign, several observatories cooperated in VLBI measurements organized jointly by the U.S. National Geodetic Survey (NGS) and the National Aeronautics and Space Administration (NASA). There were two 7-day observations arranged from Sept. 26 to Oct. 2 and from Oct. 16 to Oct. 22, with time span nearly 23 hours per day. Details of the observation and data reduction have been published elsewhere (1). This paper deals with radio source positions determined by three U.S. stations, the Haystack Observatory, the Harvard Radio Astronomy Station (HRAS) and the Owens Valley Radio Observatory (OVRO).

scholarly journals The presence of interstellar scintillation in the 15 GHz interday variability of 1158 OVRO-monitored blazars

2019 ◽  
Vol 489 (4) ◽  
pp. 5365-5380 ◽  
Author(s):  
J Y Koay ◽  
D L Jauncey ◽  
T Hovatta ◽  
S Kiehlmann ◽  
H E Bignall ◽  
...  
Keyword(s):  
Flux Density ◽  
High Energy ◽  
Short Term ◽  
Owens Valley ◽  
Hot Stars ◽  
Radio Observatory ◽  
Interstellar Scintillation ◽  
The Galaxy ◽  
Rare Class

ABSTRACT We have conducted the first systematic search for interday variability in a large sample of extragalactic radio sources at 15 GHz. From the sample of 1158 radio-selected blazars monitored over an ∼10 yr span by the Owens Valley Radio Observatory 40-m telescope, we identified 20 sources exhibiting significant flux density variations on 4-d time-scales. The sky distribution of the variable sources is strongly dependent on the line-of-sight Galactic H α intensities from the Wisconsin H α Mapper Survey, demonstrating the contribution of interstellar scintillation (ISS) to their interday variability. 21 per cent of sources observed through sightlines with H α intensities larger than 10  rayleighs exhibit significant ISS persistent over the ∼10 yr period. The fraction of scintillators is potentially larger when considering less significant variables missed by our selection criteria, due to ISS intermittency. This study demonstrates that ISS is still important at 15 GHz, particularly through strongly scattered sightlines of the Galaxy. Of the 20 most significant variables, 11 are observed through the Orion–Eridanus superbubble, photoionized by hot stars of the Orion OB1 association. The high-energy neutrino source TXS 0506+056 is observed through this region, so ISS must be considered in any interpretation of its short-term radio variability. J0616−1041 appears to exhibit large ∼20 per cent interday flux density variations, comparable in magnitude to that of the very rare class of extreme, intrahour scintillators that includes PKS0405−385, J1819+3845, and PKS1257−326; this needs to be confirmed by higher cadence follow-up observations.

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