Image of the Week

Gaia catches the movement of the tiny galaxies surrounding the Milky Way

 

Figure 1: All-sky view of orbital poles for the objects in the sample with Galactocentric distances between 100 and 200 kiloparsecs. The circles indicate the median of the 2000 Monte Carlo simulations, while the small dots around each object plot the orbital poles from the individual simulations. The magenta circles indicate a region within 10% of the assumed VPOS pole, and is indicated with an "X" for the co-orbiting direction and with a "+" for the counter-orbiting direction. Image credit: Fritz et al. 2018.

Gaia data release 2 contains proper motions for more than 1.3 billion sources, and provides a wealth of information to perform new studies on the kinematics of the Milky Way. A group of researchers lead by Tobias Fritz from the Instituto de Astrofysica de Canarias in Tenerife, Spain used the Gaia data for a new study on dwarf galaxies of the Milky Way, focusing on those dwarfs that have been spectroscopically observed in literature.

Their paper shows the power of Gaia data release 2 in a long awaited field: the determination of the tangential motions of satellite systems and, consequently, the inference of their orbital properties around the Milky Way. Such determinations for the brightest of the Milky Way satellite galaxies were the subject of one of the Gaia Collaboration papers 'Gaia Data Release 2: The kinematics of globular clusters and dwarf galaxies around the Milky Way'. With this work the sample is expanded and includes 39 dwarf galaxies out to very large distances from the Milky Way (up to 420 kiloparsecs), adding 29 galaxies, compared to previous work.

After taking into account careful selection of the sources, the systemic proper motions of the dwarf galaxies in the sample were derived. The proper motions were converted into tangential velocities in the heliocentric reference frame, after which these heliocentric tangential velocities were used together with the line-of-sight velocities to determine the total velocities in the Galactocentric reference frame, as shown in Figure 2.

Figure 2: Total velocities of all galaxies in the sample. The curves show the escape velocity for the two potentials used for this research: MWPotential14 with a NFW halo of virial mass 0.8 x 1012 Solar masses indicated with the black line, and a more massive variant with virial mass of 1.6 x 1012 Solar masses indicated with the red line. Image credit: Fritz et al. 2018.

 

Subsequently the orbital poles were calculated and other orbital parameters were deduced. The orbits of all galaxies were computed for two different Milky Way potential models: the standard MWPotential14 model, based on a spherical bulge with a disc and a NFW halo (Bovy 2015) combined with a light halo with virial mass of 0.8 x 1012 Solar masses, or combined with a heavier model with virial mass of 1.6 x 1012 Solar masses. This lead to the determination of the eccentricity, pericentre and apocentre of all galaxies for both models. Monte Carlo realizations of the orbit integrations were used to estimate the errors on the orbital parameters.

The image shown in Figure 1, featured here as the image of the week, together with the images shown in Figure 3, show the all-sky view of the orbital poles for the objects in the sample. These images focus on the objects within 200 kiloparsecs. A comparison is made of their location on this plane with the vast polar structure (VPOS) of satellites (Pawlowski et al. 2012).

 

Figure 3: All-sky view of orbital poles for the objects in the sample with Galactocentric distances between 0 and 50 kiloparsecs (top) and between 50 and 100 kiloparsecs (bottom). The circles indicate the median of the 2000 Monte Carlo simulations, while the small dots around each object plot the orbital poles from the individual simulations. The magenta circles indicate a region within 10% of the assumed VPOS pole, and is indicated with an "X" for the co-orbiting direction and with a "+" for the counter-orbiting direction. Image credit: Fritz et al. 2018.

 

The results of this research impacts several areas of knowledge of our own galaxy and its system of satellites. The mass of the Milky Way, including its dark matter halo, is still debated and can vary with more than a factor of 2 between various estimates. The motions analysed in this work suggest that the mass of the Milky Way is likely relatively high.

Furthermore, basic physics tells us that satellites should spend more time close to the apocentre of their orbits. Using this expectation, the observed distribution of orbital properties of the population of satellites suggests that there must be several dwarf galaxies not yet discovered, hiding at large distances from the Milky Way centre.

Several of the dwarf galaxy satellites of the Milky Way are found to have orbits that bring them close to the inner regions of our Galaxy, making them likely to be tidally disturbed (like they are stretched to a stream). This explains the peculiar characteristics that were observed for some of these objects. On the other hand, new questions arise, because there are satellites that do show features likely due to tidal disturbance by a large mass but that do not have orbits that seem to put them at risk of being tidally disturbed by the Milky Way.

Finally, the satellite galaxies of the Milky Way, M31, and Centaurus A appear to be preferentially arranged within thin and vast planar structures, the origin of which is still to be understood but that appear to challenge cosmological models of galaxy formation. Many of the galaxies in the sample analysed move within this planar structure. This physical property can be used by models to help explain the nature of these structures.

The paper "Gaia DR2 proper motions of dwarf galaxies within 420 kpc - Orbits, Milky Way mass, tidal influences, planar alignments, and group infall" by T.K. Fritz et al. was published today in A&A.

For this research only part of the power of Gaia Data Release 2 was used for the determination of the systemic proper motions of dwarf galaxies (given the selection of the sample was based on the requirement of having spectroscopic observations in literature for all objects). It is expected that the precisions could be improved by adding stars without existing spectroscopic measurements. Also, given that the precision in proper motion determinations by Gaia grows with the power of 1.5 of the time-baseline, it is expected that the proper motions of Gaia will be 4.5 times more accurate after the nominal mission and possibly a factor 12 more accurate for a nominal mission plus mission extension of 5 years.

An animation was created by A. Villalobos, G. Battaglia, T. Fritz making use of the NASA Milky Way rendition. This animation is available here for full interaction. Below you can find the video impression of this animation.

 

The video shows the movement of tiny galaxies surrounding the Milky Way as described in the paper: "Gaia DR2 proper motions of dwarf galaxies within 420 kpc - Orbits, Milky Way mass, tidal influences, planar alignments, and group infall" by T.K. Fritz et al. Credits: A. Villalobos, G.Battaglia, T. Fritz (animation); NASA: Milky Way rendition. Based on Fritz et al. 2018, A&A, 619, 103

 

 

See also: Press release by the Instituto de Astrofísica de Canarias - IAC

Credits: ESA/Gaia/DPAC, T. Fritz, G. Battaglia

[Published: 13/11/2018 | Updated with the animation on 29/12/2018]

Image of the Week Archive

2019
08/08: 30th anniversary of Hipparcos
17/07: Whitehead Eclipse Avoidance Manoeuvre
28/06: Following up on Gaia Solar System Objects
19/06: News from the Gaia Archive
29/05: Spectroscopic variability of emission lines stars with Gaia
24/05: Evidence of new magnetic transitions in late-type stars
03/05: Atmospheric dynamics of AGB stars revealed by Gaia
25/04: Geographic contributions to DPAC
22/04: omega Centauri's lost stars
18/04: 53rd ESLAB symposium "the Gaia universe"
18/02: A river of stars
2018
21/12: Sonification of Gaia data
18/12: Gaia captures a rare FU Ori outburst
12/12: Changes in the DPAC Executive
26/11:New Very Low Mass dwarfs in Gaia data
19/11: Hypervelocity White Dwarfs in Gaia data
15/11: Hunting evolved carbon stars with Gaia RP spectra
13/11: Gaia catches the movement of the tiny galaxies surrounding the Milky Way
06/11: Secrets of the "wild duck" cluster revealed
12/10: 25 years since the initial GAIA proposal
09/10: 3rd Gaia DPAC Consortium Meeting
30/09: A new panoramic sky map of the Milky Way's Stellar Streams
25/09: Plausible home stars for interstellar object 'Oumuamua
11/09: Impressions from the IAU General Assembly
30/06: Asteroids in Gaia Data
14/06: Mapping and visualising Gaia DR2

25/04: In-depth stories on Gaia DR2

14/04: Gaia tops one trillion observations
16/03: Gaia DR2 Passbands
27/02: Triton observation campaign
11/02: Gaia Women In Science
29/01: Following-up on Gaia
2017
19/12: 4th launch anniversary
24/11: Gaia-GOSA service
27/10: German Gaia stamp in the making
19/10: Hertzsprung-russell diagram using Gaia DR1
05/10: Updated prediction to the Triton occultation campaign
04/10: 1:1 Gaia model arrives at ESAC
31/08: Close stellar encounters from the first Gaia data release
16/08: Preliminary view of the Gaia sky in colour
07/07: Chariklo stellar occultation follow-up
24/04: Gaia reveals the composition of asteroids
20/04: Extra-galactic observations with Gaia
10/04: How faint are the faintest Gaia stars?
24/03: Pulsating stars to study Galactic structures
09/02: Known exoplanetary transits in Gaia data
31/01: Successful second DPAC Consortium Meeting
2016
23/12: Interactive and statistical visualisation of Gaia DR1 with vaex
16/12: Standard uncertainties for the photometric data (in GDR1)
25/11: Signature of the rotation of the galactic bar uncovered
15/11: Successful first DR1 Workshop
27/10: Microlensing Follow-Up
21/10: Asteroid Occultation
16/09: First DR1 results
14/09: Pluto Stellar Occultation
15/06: Happy Birthday, DPAC!
10/06: 1000th run of the Initial Data Treatment system
04/05: Complementing Gaia observations of the densest sky regions
22/04: A window to Gaia - the focal plane
05/04: Hipparcos interactive data access tool
24/03: Gaia spots a sunspot
29/02: Gaia sees exploding stars next door
11/02: A new heart for the Gaia Object Generator
04/02: Searching for solar siblings with Gaia
28/01: Globular cluster colour-magnitude diagrams
21/01: Gaia resolving power estimated with Pluto and Charon
12/01: 100th First-Look Weekly Report
06/01: Gaia intersects a Perseid meteoroid
2015
18/12: Tales of two clusters retold by Gaia
11/11: Lunar transit temperature plots
06/11: Gaia's sensors scan a lunar transit
03/11: Celebrity comet spotted among Gaia's stars
09/10: The SB2 stars as seen by Gaia's RVS
02/10: The colour of Gaia's eyes
24/09: Estimating distances from parallaxes
18/09: Gaia orbit reconstruction
31/07: Asteroids all around
17/07: Gaia satellite and amateur astronomers spot one in a billion star
03/07: Counting stars with Gaia
01/07: Avionics Model test bench arrives at ESOC
28/05: Short period/faint magnitude Cepheids in the Large Magellanic Cloud
19/05: Visualising Gaia Photometric Science Alerts
09/04: Gaia honours Einstein by observing his cross
02/04: 1 April - First Look Scientists play practical joke
05/03: RR Lyrae stars in the Large Magellanic Cloud as seen by Gaia
26/02: First Gaia BP/RP deblended spectra
19/02: 13 months of GBOT Gaia observations
12/02: Added Value Interface Portal for Gaia
04/02: Gaia's potential for the discovery of circumbinary planets
26/01: DIBs in three hot stars as seen by Gaia's RVS
15/01: The Tycho-Gaia Astrometric Solution
06/01: Close encounters of the stellar kind
2014
12/12: Gaia detects microlensing event
05/12: Cat's Eye Nebula as seen by Gaia
01/12: BFOSC observation of Gaia at L2
24/11: Gaia spectra of six stars
13/11: Omega Centauri as seen by Gaia
02/10: RVS Data Processing
12/09: Gaia discovers first supernova
04/08: Gaia flag arrives at ESAC
29/07: Gaia handover
15/07: Eclipsing binaries
03/07: Asteroids at the "photo finish"
19/06: Calibration image III - Messier 51
05/06: First Gaia BP/RP and RVS spectra
02/06: Sky coverage of Gaia during commissioning
03/04: Gaia source detection
21/02: Sky-background false detections in the sky mapper
14/02: Gaia calibration images II
06/02: Gaia calibration image I
28/01: Gaia telescope light path
17/01: First star shines for Gaia
14/01: Radiation Campaign #4
06/01: Asteroid detection by Gaia
2013
17/12: Gaia in the gantry
12/12: The sky in G magnitude
05/12: Pre-launch release of spectrophotometric standard stars
28/11: From one to one billion pixels
21/11: The Hipparcos all-sky map
15/10: Gaia Sunshield Deployment Test
08/10: Initial Gaia Source List
17/09: CU1 Operations Workshop
11/09: Apsis
26/08: Gaia arrival in French Guiana
20/08: Gaia cartoons
11/07: Model Soyuz Fregat video
01/07: Acoustic Testing
21/06: SOVT
03/06: CU4 meeting #15
04/04: DPCC (CNES) 
26/03: Gaia artist impression 
11/02: Gaia payload testing  
04/01: Space flyby with Gaia-like data
2012
10/12: DPAC OR#2. Testing with Planck
05/11: Galaxy detection with Gaia
09/10: Plot of part of the GUMS-10 catalogue
23/07: "Gaia" meets at Gaia
29/06: The Sky as seen by Gaia
31/05: Panorama of BAM clean room
29/03: GREAT school results
12/03: Scanning-law movie
21/02: Astrometric microlensing and Gaia
03/02: BAM with PMTS
12/01: FPA with all the CCDs and WFSs
2011
14/12: Deployable sunshield
10/11: Earth Trojan search
21/10: First Soyuz liftoff from the French Guiana
20/09: Fast 2D image reconstruction algorithm
05/09: RVS OMA
10/08: 3D distribution of the Gaia catalogue
13/07: Dynamical Attitude Model
22/06: Gaia's view of open clusters
27/05: Accuracy of the stellar transverse velocity
13/05: Vibration test of BAM mirrors
18/04: L. Lindegren, Dr. Honoris Causa of the Observatory of Paris
19/01: Detectability of stars close to Jupiter
05/01: Delivery of the WFS flight models
2010
21/12: The 100th member of CU3
17/11: Nano-JASMINE and AGIS
27/10: Eclipsing binary light curves fitted with DPAC code
13/10: Gaia broad band photometry
28/09: Measuring stellar parameters and interstellar extinction
14/09: M1 mirror
27/08: Quest for the Sun's siblings
 
Please note: Entries from the period 2003-2010 are available in this PDF document.