Miripedia

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mybb@mybb.ru (��2) — Sun, 31 May 2020 13:29:33 +0300

https://space.skyrocket.de/doc_sdat/tks-va.htm

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https://space.skyrocket.de/doc_sat/sts_hist.htm

https://en.wikipedia.org/wiki/RS-25#/me … istory.png

http://www.pereplet.ru/space/hotnews/18.02.99.html

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mybb@mybb.ru (��1) — Tue, 03 Sep 2019 11:06:22 +0300

https://elementy.ru/novosti_nauki/43167 … na_planete

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mybb@mybb.ru (��1) — Mon, 02 Sep 2019 00:39:41 +0300

https://en.wikipedia.org/wiki/Periodic_table

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List of the most distant astronomical objects

mybb@mybb.ru (��1) — Mon, 02 Sep 2019 00:33:40 +0300

https://en.wikipedia.org/wiki/List_of_t … al_objects

ZTF

mybb@mybb.ru (��1) — Sat, 31 Aug 2019 19:26:40 +0300

https://www.ztf.caltech.edu/news/public-data-release-1

ZTF PUBLIC DATA RELEASE 1: Available NOW, May 8, 2019.

The Zwicky Transient Facility (ZTF) and IPAC at the California Institute of Technology announce the first ZTF Public Data Release. ZTF is an optical time-domain survey covering the northern sky visible from Palomar Observatory. This release includes data products from the public portion of the survey spanning March to December, 2018. The products include ~3.4 million single-exposure images, ~102 thousand co-added images, accompanying source catalog files containing ~63 billion sources detected from those images, and ~2 billion lightcurves constructed from the single-exposure extractions. Note: transient alerts extracted from difference-images commenced public distribution on June 4, 2018. These alerts continue to be generated and distributed as the public survey proceeds.

�� TESS

mybb@mybb.ru (��1) — Fri, 30 Aug 2019 23:46:06 +0300

https://tsc.mit.edu/talks/Matthew Holman.pdf

�� (��)

mybb@mybb.ru (��1) — Fri, 30 Aug 2019 22:18:49 +0300

https://za-neptunie.livejournal.com/333988.html

�� 1061

https://en.wikipedia.org/wiki/Gliese_1061

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VVV

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 21:48:49 +0300

https://arxiv.org/abs/1809.05167

VVV Survey Microlensing: the Galactic Longitude Dependence

We completed the search for microlensing events in the zero latitude area of the Galactic bulge using the VVV Survey near-IR data obtained between 2010 and 2015. We have now a total sample of N = 630 events Using the near-IR Color-Magnitude Diagram we selected the Red Clump sources to analyze the longitude dependence of microlensing across the central region of the Galactic plane. The events show a homogeneous distribution, smoothly increasing in numbers towards the Galactic centre, as predicted by different models. We find a slight asymmetry, with a larger number of events toward negative longitudes than positive longitudes. This asymmetry is seen both in the complete sample and the subsample of red clump giant sources, and it is possibly related with the inclination of the bar along the line of sight. The timescale distribution is fairly symmetric with a peak in 17.4 � 1.0 days for the complete sample (N = 630 events), and 20.7 � 1.0 days for the Red Clump stars (N = 291 events), in agreement with previous results.

https://arxiv.org/abs/1807.04303

Deep near-IR images from the VVV Survey were used to search for RR Lyrae type ab (RRab) stars within 100' from the Galactic Centre (GC). A sample of 960 RRab stars were discovered.

SuperWASP

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 21:29:06 +0300

https://www.zooniverse.org/projects/ajn … able-stars

All 1.5 million+ folded lightcurves are now uploaded to the project and ready for classification.

https://arxiv.org/abs/1707.02045

The SuperWASP catalogue of 4963 RR Lyr stars: identification of 983 Blazhko effect candidates

The SuperWASP RRab catalogue consists of 4963 objects of which 3397 are previously unknown. We discovered 983 distinct candidates for Blazhko effect objects, 613 of these being previously unknown in the literature as RR Lyrae stars, and 894 are previously unknown to be Blazhko effect stars.

Objects are identified using the USNO-B1.0 input catalogue and given a unique 1SWASP identifier (SWASPid) based on these coordinates. The
archive contains over 31 million objects.

ASAS-SN (All-Sky Automated Survey for Supernovae)

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 21:18:20 +0300

https://za-neptunie.livejournal.com/239767.html

https://arxiv.org/pdf/1704.02320.pdf

ATLAS

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 16:19:53 +0300

http://atlas.fallingstar.com/ua20180305.php

During its first two years ATLAS observed 140 million stars hundreds of times and has detected variability (pulsation, rotation, occultations, outbursts) in 5 million objects. We will be releasing these light-curves through the Mikulski Archive for Space Telescopes. The ensuing 6 months has doubled the number of detections and increased the number of stars to 240 million. There will be periodic data releases and updates.

Catalina

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 16:09:05 +0300

http://iawn.net/documents/201401_1st_Ca … en_css.pdf

Current Facilites

Mt. Bigelow, AZ 0.7-m Schmidt 8.2 sq.deg. FOV Vlim~19.5 ~250 NEOs/year
Mt. Lemmon, AZ 1.5-m reflector 1.2 sq.deg. FOV Vlim~21.3 ~350 NEOs/year

Retired Facilites

Siding Spring Observatory, Australia 0.5-m Uppsala Schmidt 4.2 sq. deg. FOV Vlim ~ 19.0 2004 � 2013 ~50 NEOs/year

Increased FOV for both CSS survey telescopes

G96 1.2 deg2 -> 5.0 deg2 (~1,100 sq deg2/night)
703 8.2 deg2 -> 19.4 deg2 (~4,300 sq deg2/night)

Proposed FaciliKes
� CLASS: the Catalina LCOGT Asteroid Southern Survey
� 3 x 1.0-m telescopes, 25 sq. deg FOV equivalent
� Flexible operation � can survey separately or together
� ~5800 sq. deg. coverage per night to V~20.4, or ~2000 sq. deg. to V~21.6 (assuming 4 visits)
� To be located on Cerro Tololo, Chile

http://adsabs.harvard.edu/abs/2014DPS....4641409J

The 1.0m follow-up telescope on Mt. Lemmon is now operational (MPC code I52) and providing asteroid astrometry. A new camera for the 1.5 m telescope (G96) will increase the field four times to 5 square degrees and may be operational by the end of the year. A similar camera for the Catalina Schmidt telescope (703) will follow with a 19.4 square degree field. These upgrades will substantially increase the NEO discovery rate from CSS. Additionally, software upgrades to accommodate the larger data flow are in process.

Gaia

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 15:26:03 +0300

https://arxiv.org/abs/1811.05301

Abstract: The source detection sensitivity of Gaia is reduced near sources. To characterise this contrast sensitivity is important for understanding the completeness of the Gaia data products, in particular when evaluating source confusion in less well resolved surveys, such as in photometric monitoring for transits. Here, we statistically evaluate the catalog source density to determine the Gaia Data Release 2 source detection sensitivity as a function of angular separation and brightness ratio from a bright source. The contrast sensitivity from 0.4 arcsec out to 12 arcsec ranges in DG = 0-14 mag. We find the derived contrast sensitivity to be robust with respect to target brightness, colour, source density, and Gaia scan coverage.

https://arxiv.org/abs/1811.04302

The nearest extreme velocity stars among Gaia DR2 high proper motion stars

Among about 1.8 million Gaia DR2 high proper motion stars with μ>60 mas/yr and moderately significant parallaxes (ϖ>3σϖ), we have selected 109 high-speed star candidates with Galactic rest frame tangential velocities (corrected for solar motion) vt,g>700 km/s, well above the local Galactic escape velocity. After applying various Gaia DR2 astrometric quality criteria, only 39 candidates remained, including all three hypervelocity runaway white dwarfs (HVR WDs) found by Shen et al. (2018) but no additional such candidates (falling in the same region of the colour-magnitude diagram).

https://arxiv.org/abs/1810.09489

OGLE Collection of Galactic Cepheids

We present here a new major part of the OGLE Collection of Variable Stars - OGLE Collection of Galactic Cepheids. The new dataset was extracted from the Galaxy Variability Survey images - a dedicated large-scale survey of the Galactic disk and outer bulge conducted by the OGLE project since 2013.
The OGLE collection contains 2718 Cepheids of all types - classical, type II and anomalous. It more than doubles the number of known Galactic classical Cepheids. Due to the long-term monitoring and large number of epochs the selected sample is very pure, generally free from contaminating stars of other types often mimicking Cepheids. Its completeness is high at 90% level for classical Cepheids - tested using recent samples of Galactic Cepheids: ASAS-SN, ATLAS, Gaia DR2 and Wise catalog of variable stars. Our comparisons indicate that the completeness of the two latter datasets, Gaia DR2 and Wise catalog, is very low, at < 10% level in the magnitude range of the OGLE GVS survey (10.8 < I < 19.5 mag). Both these samples are severely contaminated by non-Cepheids (the purity is 67% and 56%, respectively).
We also present several interesting objects found in the new OGLE Collection - multi-mode pulsators, a first Galactic candidate for eclipsing system containing Cepheid, a binary Cepheid candidate.

https://arxiv.org/abs/1805.02079

Gaia Data Release 2: Specific characterisation and validation of all-sky Cepheids and RR Lyrae stars

Multiband time series photometry and characterisation by the SOS Cep&RRL pipeline are published in Gaia DR2 for 150,359 such variables (9,575 classified as Cepheids and 140,784 as RR Lyrae stars) distributed all over the sky. The sample includes variables in 87 globular clusters and 14 dwarf galaxies. To the best of our knowledge, as of 25 April 2018, variability of 50,570 of these sources (350 Cepheids and 50,220 RR Lyrae stars) is not known in the literature, hence likely they are new discoveries by Gaia. An estimate of the interstellar absorption is published for 54,272 fundamental-mode RR Lyrae stars from a relation based on the G-band amplitude and the pulsation period. Metallicities derived from the Fourier parameters of the light curves are also released for 64,932 RR Lyrae stars and 3,738 fundamental-mode classical Cepheids with period shorter than 6.3 days.

https://arxiv.org/abs/1805.02035

Gaia Data Release 2: The first Gaia catalogue of long-period variable candidates

Gaia DR2 provides a unique all-sky catalogue of 550'737 variable stars, of which 151'761 are long-period variable (LPV) candidates with G variability amplitudes larger than 0.2 mag (5-95% quantile range). About one-fifth of the LPV candidates are Mira candidates, the majority of the rest are semi-regular variable candidates. For each source, G, BP , and RP photometric time-series are published, together with some LPV-specific attributes for the subset of 89'617 candidates with periods in G longer than 60 days.

https://arxiv.org/abs/1804.09365

Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars.

OGLE

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 15:02:08 +0300

https://arxiv.org/abs/1810.09489

OGLE Collection of Galactic Cepheids

https://arxiv.org/abs/1807.00008

The OGLE Collection of Variable Stars. Type II Cepheids in the Magellanic System

We present a nearly complete collection of type II Cepheids in the Magellanic System. The sample consists of 338 objects: 285 and 53 variables in the Large and Small Magellanic Clouds, respectively. Based on the pulsation periods and light-curve morphology, we classified 118 of our type II Cepheids as BL Herculis, 120 as W Virginis, 34 as peculiar W Virginis, and 66 as RV Tauri stars. For all objects, we publish time-series VI photometry obtained during the OGLE-IV survey, from 2010 to the end of 2017.

https://arxiv.org/abs/1701.03105

The OGLE Collection of Variable Stars. Over 450 000 Eclipsing and Ellipsoidal Binary Systems Toward the Galactic Bulge

We present a collection of 450 598 eclipsing and ellipsoidal binary systems detected in the OGLE fields toward the Galactic bulge. The collection consists of binary systems of all types: detached, semi-detached, and contact eclipsing binaries, RS CVn stars, cataclysmic variables, HW Vir binaries, double periodic variables, and even planetary transits. For all stars we provide the I- and V-band time-series photometry obtained during the OGLE-II, OGLE-III, and OGLE-IV surveys. We discuss methods used to identify binary systems in the OGLE data and present several objects of particular interest.

https://arxiv.org/abs/1612.06394

The OGLE Collection of Variable Stars. Eclipsing Binaries in the Magellanic System

We present the collection of eclipsing binaries in the Large and Small Magellanic Clouds, based on the OGLE survey. It contains 48605 systems, 40204 belonging to the LMC and 8401 to the SMC. Out of the total number of the presented binaries, 16374 are the new ones. We present the time-series photometry obtained for the selected objects during the fourth phase of the OGLE project. The catalog has been created using a two step machine learning procedure based on the Random Forest algorithm.

HATPI

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 13:19:05 +0300

https://hatpi.org/science/

http://fornaxmounts.com/science.html

The HAT-PI Project is building a telescope that will, in a single exposure, observe the majority of the night sky visible from its observing site in Chile in 30 seconds. This is accomplished by attaching up to 63 carefully aligned lens-and-camera sub-units to a large mount. The mount will track stars as they rise and set during the night while the telescope keeps imaging, effectively creating a movie of the night-sky. HAT-PI will enable the detection of a diverse array of objects ranging from near-earth asteroids and exoplanets around bright stars to novae and bright gamma-ray bursts. The large field of view of this instrument, coupled with the dense time-sampling, will vastly improve our understanding of transient astronomical events.

https://web.astro.princeton.edu/news/ga … pi-project

Wednesday, May 3, 2017

Principal Investigator Gaspar Bakos has been awarded $1M through the Gordon and Betty Moore Foundation for a project at Princeton dubbed HATPI � �HAT� from the Hungarian-made Automated Telescope and �PI� for the sky coverage of the telescope (π steradians) of the night sky � about the angle covered by an umbrella held over your head.

While most telescopes make very specific observations, repeated with a timescales of a few days to years, HATPI has a 30-second cadence through a hedgehog-like array of 63 telescopes on a single mount. HATPI will create very high precision measurements to detect the shadow of a planet crossing the (unseen) disk of nearby stars. It is also great for finding earth-threatening asteroids, all kinds of variable stars, exploding stars and possibly even the optical emission from a gravitational wave source. The telescope will be sited at Las Campanas Observatory in northern Chile. It will cover the whole sky every clear night and over the course of a year, it will record three-quarters of the entire sky. The Princeton team also aims to process the data in real time and make the results public.

https://arxiv.org/pdf/1801.00849.pdf

In parallel to TESS, we anticipate that a new ground-based survey, called HATPI, will come online. HATPI will ultimately use an array of 63 lenses and CCDs to image the entire sky above 30 degrees (1 π steradian) on a mosaic, every 30 seconds, whenever conditions permit, yielding better than 3 mmag photometric precision at 30 s cadence for stars at r ≈ 10. Construction of HATPI at Las Campanas Observatory
is under way. The massive, high-precision data from HATPI will complement TESS, and will also offer remarkable synergies with the Gaia space mission.

Evryscope

mybb@mybb.ru (��1) — Wed, 14 Nov 2018 13:04:14 +0300

http://evryscope.astro.unc.edu/

https://twitter.com/evryscopectio

http://icc.ub.edu/webs/ICCUB_Winter_Meeting/sites/icc.ub.edu.webs.ICCUB_Winter_Meeting/files/Octavi Fors.pdf

Bright targets:
2650 Hot Subdwarfs (Geier 2017)
2100 WDs (~full list until Gaia-DR2)
Results:
Two new HSDs reflecion binaries
No WDs transits / debris disks (yet)

Example low-mass eclipsing binary / hot Jupiter

Evryscope South Database
250TB raw data collected so far
Total imaging data ~1PB/year
1.4x107 light curves down to g�~15mag
4x1011 photometric measurements (~1x109 per night)

https://arxiv.org/abs/1807.09806
Young and eccentric: the quadruple system HD 86588

https://arxiv.org/abs/1804.02001

Evryscope detects a superflare from Proxima Centauri

https://arxiv.org/abs/1501.03162

Evryscope science: exploring the potential of all-sky gigapixel-scale telescopes

https://arxiv.org/abs/1407.0026

The Evryscope: the first full-sky gigapixel-scale telescope

https://twitter.com/vacant3rdman/status … 4888150017

9:24 - 11 ��. 2018 �.

Evryscope data not currently public, but would like to make it so. Currently trying to work out how best to make 40TB of light curves accessible... #SPIEastro

�� QUEST � ESO

mybb@mybb.ru (��1) — Tue, 13 Nov 2018 21:31:52 +0300

https://arxiv.org/abs/1603.07673
First Results from the La Silla-QUEST Supernova Survey and the Carnegie Supernova Project

https://arxiv.org/abs/1210.1584
La Silla-QUEST Variability Survey in the Southern Hemisphere

https://arxiv.org/abs/1208.4599
The QUEST RR Lyrae Survey: III. The Low Galactic Latitude Catalogue

https://arxiv.org/abs/1205.5214
The La Silla - QUEST Kuiper Belt Survey
In a survey covering ~7500 deg2, we have thus far detected 77 KBOs and Centaurs, more than any other full-hemisphere search to date. Using a pattern of dithered pointings, we demonstrate a search efficiency exceeding 80%.

�� SkyMapper

mybb@mybb.ru (��1) — Tue, 13 Nov 2018 20:52:43 +0300

https://news.mb.com.ph/2017/04/05/astro … -planet-9/

Australian National University (ANU) releases data from their 14-square-foot SkyMapper telescope at the Siding Spring Observatory to the public, and 60,000 citizen scientists have examined the data to hunt for planets. SkyMapper was trained on the outskirts of the universe: the Trans-Neptunian Objects (TNOs), which lie beyond Neptune and include Pluto, the Kuiper Belt and the Oort Cloud.

�We�ve managed to rule out a planet about the size of Neptune being in about 90 percent of the southern sky out to a depth of about 350 times the distance the Earth is from the sun,� lead researcher and ANU astrophysicist Brad Tucker said in a statement.

�With the help of tens of thousands of dedicated volunteers sifting through hundreds of thousands of images taken by SkyMapper, we have achieved four years of scientific analysis in under three days.�

�It�s actually not that complicated to find Planet Nine. It really is spot the difference. Then you just click on the image, mark what is different and we�ll take care of the rest,� he said. The four objects found by the citizen astronomers are still under study, and little is known about them.

http://astro.tsinghua.edu.cn/~xbai/teac … Mapper.pdf

3.1, What Is the Distribution of Solar System Objects
Beyond Neptune?
---- quiescent comet-like objects
---- Trans-Neptunian Object (TNO)
Two epochs ~4 hours on the first night
A third epoch 1-3 days later
A fourth epoch after 1 month

http://www.astro.lu.se/~louise/Louise_SFA.pdf

Searching for Trans-Neptunian Objects
� Predicted to find around 2000 TNOs across the sky.

http://skymapper.anu.edu.au/surveys/

Progress survey

�� Thacher

mybb@mybb.ru (��1) — Sun, 11 Nov 2018 16:11:42 +0300

http://adsabs.harvard.edu/abs/2017AAS...22914704E

https://za-neptunie.livejournal.com/284612.html

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�� ESO

mybb@mybb.ru (��1) — Sun, 11 Nov 2018 15:59:57 +0300

http://archive.eso.org/wdb/wdb/eso/sche … 297.C-5014(A)

Precise Search for Planet 9 : Q3

PI: laskar , Jacques

Abstract: In January 2016, Batygin and Brown have proposed the existence of an additional Planet 9 (P9) in our solar system for explaining the distribution of the Kuiper Belt Objects (KBO). As they consider the long term effect of P9 on the KBO, they cannot constrain its longitude and search for P9 in a large band of about $7200 \,\rm{deg}^2$. On the opposite, we are using the same method that led Le Verrier to the discovery of Neptune. Using our high precision model for the solar system, we compute the deformation that P9 would cause on the orbit of Saturn. We fit the full solar system parameters and analyse the residuals in the Cassini data that provide an Earth-Saturn distance with a 70 meter accuracy (Fienga et al. 2016). The minimisation of the residuals allows us to directly obtain the location of P9 in 4 isolated possible spots (Q1,Q2,Q3,Q4). This proposal is to scan the 12 $\rm{deg}^2$ central part of Q3, the only P9 spot that is observable by the VST in P96, to detect Planet 9.

Run ID: 297.C-5014(A)
Publication(s): N/A

http://archive.eso.org/wdb/wdb/eso/sche … 098.C-0542(A)

http://archive.eso.org/wdb/wdb/eso/sche … 098.C-0542(B)

http://archive.eso.org/wdb/wdb/eso/sche … 098.C-0542(C)

Precise Search for Planet 9

PI: laskar , Jacques

Abstract: In January 2016, Batygin and Brown have proposed the existence of an additional Planet 9 (P9) in our solar system for explaining the distribution of the Kuiper Belt Objects (KBO). As they consider the long term effect of P9 on the KBO, they cannot constrain the longitude of P9. Their strategy is then to scan a large band in the sky of about $20\times 360 = 7200 \rm{deg}^2$. On the opposite, we are using the same method that led Le Verrier to the discovery of Neptune. Using our high precision model for the solar system, we compute the deformation that P9 would cause on the orbit of Saturn. We fit the full solar system parameters and analyse the residuals in the Cassini data that provide an Earth-Saturn distance with a 70 meter accuracy (Fienga et al. 2016). The minimisation of the residuals allows us to directly obtain the location of P9 in a few isolated possible spots. This proposal is to scan the only $35 \rm{deg}^2$ P9 spot that is observable by the VST in P98, to detect Planet 9.

Run ID: 098.C-0542(C)
Publication(s): N/A

�� .��

mybb@mybb.ru (��1) — Sun, 11 Nov 2018 14:38:10 +0300

https://www.space.com/31677-astronomers … -nine.html
January 21, 2016

"Even at its most distant, and at the smallest guesses of how big it is, it's like 24th or 25th magnitude," Brown said, referring to the brightness scale astronomers use, in which higher numbers denote fainter objects. "It's not crazy; this is the kind of stuff people are finding all the time. We just need to go out and cover a good swathe of the sky."

Just how big a swathe? Astronomer Scott Sheppard, of the Carnegie Institution for Science in Washington, D.C., has come up with a rough estimate: between 2,000 and 4,000 square degrees. (For perspective, the full moon as seen from Earth covers about 0.5 degrees of sky.)

That corresponds to about 50 nights of observations using a powerful instrument such as the Subaru Telescope in Hawaii, said Sheppard, who has a lot of experience finding far-flung objects in the solar system. For example, in 2014, he and Chadwick Trujillo of the Gemini Observatory in Hawaii discovered an object called 2012 VP113, whose orbital characteristics hint at the presence of a Planet Nine.

https://www.scientificamerican.com/arti … st-planet/
October 25, 2016

"However, these estimates still leave a swath of sky "about 1,500 square degrees large," says astronomer Scott Sheppard at the Carnegie Institution for Science, who with astronomer Chadwick Trujillo first suggested the existence of Planet Nine in 2014. (In comparison, the full moon as seen from Earth covers about 0.2 degrees of sky.) This swath described by Sheppard corresponds to about 20 nights of observations on Subaru, "and if we get seven nights or so this year, that's three years�if it's not rainy any of those nights," Sheppard says.
So the strategy in the race is now largely a matter of reducing the search area by eliminating theoretical possibilities. In an as-yet unpublished set of about 100 new high-resolution computer simulations, Batygin says he and Brown have narrowed down Planet Nine's location to a roughly 600- to 800-square degree patch of sky. They first modeled the solar system over the course of about 4 billion years, focusing on how the gravitational pulls of the system�s largest planets�Jupiter, Saturn, Uranus, Neptune and Planet Nine�might have sculpted the orbits of thousands of randomly scattered Kuiper Belt objects (KBOs). "We're searching for all of the things that Planet Nine does to the solar system," Brown says."

https://arxiv.org/pdf/1603.05712.pdf

We began a survey of these regions in the fall of 2015 and will attempt to cover all of this part of the predicted orbital path.

https://www.naoj.org/Observing/Schedule/s16b.html

S16B-049, Fumi Yoshida et al.,
Hunting Planet Nine and RR-Lyrae stars in the Milky Way halo with HSC
HSC, 3 nights, abstract

https://www.naoj.org/Observing/Schedule … 6B-049.txt

(Proposal ID) S16B-049

(PI) Yoshida, Fumi

(Proposal Title)
Hunting Planet Nine and RR-Lyrae stars in the Milky Way halo with HSC

(Abstract)
We request 20 nights to conduct an HSC g-band cadence observation (2 visits per night and 8 visits of the same field in total) over ~800 sq. degrees in order to hunt down the theoretically predicted giant planet, "Planet Nine". The combination of large aperture, wide field-of-view, and exquisite image quality of HSC/Subaru enables us to reach the required depth of 25~mag (AB) with 90~sec exposure for each visit, allowing us to cover the entire high-probability regions where Planet Nine should be currently located. Planet Nine, if discovered, promises to revolutionize our knowledge of the origin of the solar system, the physics of giant planets, and the connection to exoplanetary systems. In addition to this high-risk, high-return scientific goal, the same data will allow us to carry out the following guaranteed science: discovery of ~0.2M main-belt objects and ~10^4 Kuiper-belt objects in this previously unexplored region, in addition to the discovery of more than 1,500 RR-Lyrae (RRL) stars in the halo region of the Milky-Way (MW), about 100 of which will lie at distances in the range 100-700kpc (the virial radius of the MW is ~300kpc). The distribution of RRL stars will allow us to study the structure of the MW dark matter halo and to possibly detect its outer edge.

https://www.naoj.org/Observing/Schedule/s17b.html

S17B-044 Fumi Yoshida Hunting Planet Nine and RR-Lyrae stars with HSC HSC 1.5

https://www.naoj.org/Observing/Schedule/s18b.html

S18B-071 Fumi Yoshida Hunting Planet Nine and RR-Lyrae stars with HSC HSC 3

12 �� 2015
4 �� 2016
26-29 �� 2016 �� (�� )
3-4 �� 2016 �� (�� )
21-25 �� 2017 (�� )
15 �� 2017 �� (�� )
16-17 �� 2017 �� (�� , �� )
21 �� 2018 �� (�� )
8-10 �� 2018 �� (�� )
1-4 �� 2018 �� (�� )
7 � 9 �� 2018 �� (�� )
3-9 �� 2018 �� (�� 8 ��) (��-�� ?)

https://www.space.com/42177-when-will-w … -nine.html

October 18, 2018 07:30am ET

Indeed, the search has so far covered just 20 percent to 25 percent of "premium sky," the regions where Planet Nine is most likely to be, both Sheppard and Batygin said.

�� !

mybb@mybb.ru (��2) — Thu, 08 Nov 2018 08:09:35 +0300

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mybb@mybb.ru (��1) — Thu, 01 Nov 2018 20:23:44 +0300

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