J/A+A/669/L3 Photometry data of (136199) Eris (Szakats+, 2023)
Tidally locked rotation of the dwarf planet (136199) Eris discovered via
long-term ground-based and space photometry.
Szakats R., Kiss Cs., Ortiz J.L., Morales N., Pal A., Muller T.G.,
Greiner J., Santos-Sanz P., Marton G., Duffard R., Sagi P., Forgacs-Dajka E.
<Astron. Astrophys. 669, L3 (2023)>
=2023A&A...669L...3S 2023A&A...669L...3S (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets ; Photometry ; Optical
Keywords: Kuiper belt objects: individual: (136199) Eris -
methods: observational - techniques: photometry
Abstract:
The rotational states of the members in the dwarf planet - satellite
systems in the transneptunian region are determined by the formation
conditions and the tidal interaction between the components, and these
rotational characteristics are the prime tracers of their evolution.
Previously a number of authors claimed highly diverse values for the
rotation period for the dwarf planet Eris, ranging from a few hours to
a rotation (nearly) synchronous with the orbital period (15.8d) of its
satellite, Dysnomia. In this letter we present new light curve data of
Eris, taken with ∼1-2m-class ground based telescopes, and with the
TESS and Gaia space telescopes.
TESS data could not provide a well-defined light curve period, but
could constrain light curve variations to a maximum possible light
curve amplitude of dm≤0.03mag (1-sigma) for P≤24h periods.
Both the combined ground-based data and the Gaia measurements
unambiguously point to a light curve period equal to the orbital
period of Dysnomia, P=15.8d, with a light curve amplitude of
dm∼0.03mag, i.e. the rotation of Eris is tidally locked. Assuming that
Dysnomia has a collisional origin, calculations with a simple tidal
evolution model show that Dysnomia has to be relatively massive (mass
ratio of q=0.01-0.03) and large (radius of Rs≥300km) to slow down
Eris to synchronized rotation. These simulations also indicate that
- assuming tidal parameters usually considered for transneptunian
objects - the density of Dysnomia should be 1.8-2.4g/cm3, an
exceptionally high value among similarly sized transneptunian objects,
putting important constraints on the formation conditions.
Description:
Collected photometry data from Gaia space observatory, TESS and from
ground based telescopes, e.g. MPG 2.2m (GROND), La Hita 0.77m, CA2.2
(CAFOS2.2) and 1.5m telescope at Observatorio de Sierra Nevada.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 30 215 TESS Photometry of Eris
tablea2.dat 54 111 Ground based photometry of Eris
tablea4.dat 32 415 Gaia Photometry of Eris
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Byte-by-byte Description of file:tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d JD Julian Date of observation, UTC
15- 22 F8.5 mag Tmag Brightness (TESS bandpass)
24- 30 F7.5 mag e_Tmag Uncertainty of brightness
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Inst Telescope/Instrument
(1.5m, CA2.2, GROND or LaHita)
9- 21 F13.5 d JD Julian Date of observation; UTC
24- 29 F6.3 mag mag Brightness in Filter (1)
32- 36 F5.3 mag e_mag Uncertainty of brightness
39- 40 A2 --- Filt Filter (2)
43- 47 F5.1 min Texp Exposure time
50- 54 F5.1 min Ttot Total observing time
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Note (1): GROND data is in the AB system.
Note (2): Filters as:
1.5m : C and R
CA2.2 : R
GROND : H, J, g', i', r'. z'
LaHita : C
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d JD Julian Date of observation, UTC
16- 23 F8.5 mag Gmag Corrected Brightness (Gaia G bandpass)
26- 32 F7.5 mag e_Gmag Uncertainty of brightness
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Acknowledgements:
Robert Szakats, szakats.robert(at)csfk.org
(End) Robert Szakats [Konkoly Obs., Hungary], Patricia Vannier [CDS] 30-Nov-2022