Detection of H<i>α</i> emission from PZ Telescopii B using SPHERE/ZIMPOL

Barcucci, A. Musso; Cugno, Gabriele; Launhardt, R.; Müller, André; Szulágyi, J.; Boekel, R. van; Henning, Thomas; Bonnefoy, M.; Quanz, Sascha P.; Cantalloube, F.

doi:10.1051/0004-6361/201936510

Cited by 6 publications

(9 citation statements)

References 46 publications

(73 reference statements)

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“…a L e ) is therefore expected to have a chromospheric origin instead of accretion, which seems also likely given the age of 24 Myr (Musso Barcucci et al 2019). That interpretation is consistent with the lack of reddening in the M′ band (see Stolker et al 2020b and Figure 9).…”

Section: ~-supporting

confidence: 58%

“…Figure 9 shows L Hα versus H − M′. Here, we have adopted the available magnitudes and line fluxes from species for PDS 70 b (Hashimoto et al 2020;Stolker et al 2020a), GSC 06214 B (Ireland et al 2011;Bailey et al 2013;Zhou et al 2014), PZ Tel B (Biller et al 2010;Musso Barcucci et al 2019;Stolker et al 2020b), HD 142527 B (Biller et al 2012Lacour et al 2016;Cugno et al 2019), and GQ Lup B (this work). Extinction effects are typically nonnegligible during formation, especially at optical wavelengths, but can also be quite uncertain.…”

Section: Hα-color Characteristics Of Directly Imaged Planets and Low-...mentioning

confidence: 99%

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Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*

Stolker

Haffert

Kesseli

et al. 2021

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GQ Lup B is a young and accreting, substellar companion that appears to drive a spiral arm in the circumstellar disk of its host star. We report high-contrast imaging observations of GQ Lup B with VLT/NACO at 4–5 μm and medium-resolution integral field spectroscopy with VLT/MUSE. The optical spectrum is consistent with an M9 spectral type, shows characteristics of a low-gravity atmosphere, and exhibits strong Hα emission. The H − M′ color is ≳1 mag redder than field dwarfs with similar spectral types, and a detailed analysis of the spectral energy distribution (SED) from optical to mid-infrared wavelengths reveals excess emission in the L′, NB4.05, and M′ bands. The excess flux is well described by a blackbody component with T disk ≈ 460 K and R disk ≈ 65 R J and is expected to trace continuum emission from small grains in a protolunar disk. We derive an extinction of A V ≈ 2.3 mag from the broadband SED with a suspected origin in the vicinity of the companion. We also combine 15 yr of astrometric measurements and constrain the mutual inclination with the circumstellar disk to 84 ± 9 deg, indicating a tumultuous dynamical evolution or a stellar-like formation pathway. From the measured Hα flux and the estimated companion mass, M p ≈ 30 M J, we derive an accretion rate of M ̇ ≈ 10 − 6.5 M J yr − 1 . We speculate that the disk is in a transitional stage in which the assembly of satellites from a pebble reservoir has opened a central cavity while GQ Lup B is in the final stages of its formation.

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Section: ~-supporting

confidence: 58%

Section: Hα-color Characteristics Of Directly Imaged Planets and Low-...mentioning

confidence: 99%

Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*

Stolker

Haffert

Kesseli

et al. 2021

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“…Hα emission thought to be originating from chromospheric activity has been observed in a number of BDs. Recent examples include the more massive BD companion PZ TEL B (Musso Barcucci et al 2019) and a survey of Sco-Cen BDs by Petrus et al (2020), but typically with lower levels of emission than we find for Delorme 1 (AB)b. Manara et al (2013) obtained an analytical relation from observations of a number of young (<10 Myr) K7 -M9.5 stars and BDs for the purpose of estimating the chromospheric activity contribution as an accretion-luminosity noise.…”

Section: Appendix A: Muse Data Reduction and Chromospheric Activitymentioning

confidence: 46%

Strong Hα emission and signs of accretion in a circumbinary planetary mass companion from MUSE

Eriksson

Torres

Janson

et al. 2020

A&A

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Context. Intrinsic Hα emission can be advantageously used to detect substellar companions because it improves contrasts in direct imaging. Characterising this emission from accreting exoplanets allows for the testing of planet formation theories. Aims. We characterise the young circumbinary planetary mass companion 2MASS J01033563-5515561 (AB)b (Delorme 1 (AB)b) through medium-resolution spectroscopy. Methods. We used the new narrow-field mode for the MUSE integral-field spectrograph, located on the ESO Very Large Telescope, during science verification time to obtain optical spectra of Delorme 1 (AB)b. Results. We report the discovery of very strong Hα and Hβ emission, accompanied by He I emission. This is consistent with an active accretion scenario. We provide accretion rate estimates obtained from several independent methods and find a likely mass of 12−15 MJup for Delorme 1 (AB)b. This is also consistent with previous estimates. Conclusions. Signs of active accretion in the Delorme 1 system might indicate a younger age than the ∼30−40 Myr expected from a likely membership in Tucana-Horologium (THA). Previous works have also shown the central binary to be overluminous, which gives further indication of a younger age. However, recent discoveries of active discs in relatively old (∼40 Myr), very low-mass systems suggests that ongoing accretion in Delorme 1 (AB)b might not require in and of itself that the system is younger than the age implied by its THA membership.

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“…Similarly to Cugno et al (2019), in order to estimate the stellar flux in the continuum filter, we calculated the median of the count rate in an aperture of radius 1.5 arcsec and applied it in Eq. 4 from Schmid et al (2017) after subtracting the background calculated in a ring at r = 1 (see Musso Barcucci et al 2019). The filter zero point was also taken from Schmid et al (2017).…”

Section: Analysis and Resultsmentioning

confidence: 99%

The widest Hα survey of accreting protoplanets around nearby transition disks

Zurlo

Cugno

Montesinos

et al. 2020

A&A

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Context. The mechanisms of planet formation are still under debate. We know little about how planets form, even if more than 4000 exoplanets have been detected to date. Recent investigations target the cot of newly born planets: the protoplanetary disk. At the first stages of their life, exoplanets still accrete material from the gas-rich disk in which they are embedded. Transitional disks are indeed disks that show peculiarities, such as gaps, spiral arms, and rings, which can be connected to the presence of substellar companions. Aims. To investigate what is responsible for these features, we selected all the known transitional disks in the solar neighborhood (<200 pc) that are visible from the southern hemisphere. We conducted a survey of 11 transitional disks (TDs) with the SPHERE instrument at the Very Large Telescope. This is the largest Hα survey that has been conducted so far to look for protoplanets. The observations were performed with the Hα filter of ZIMPOL in order to target protoplanets that are still in the accretion stage. All the selected targets are very young stars, less than 20 Myr, and show low extinction in the visible. Methods. We reduced the ZIMPOL pupil stabilized data by applying the method of the angular spectral differential imaging (ASDI), which combines both techniques. The datacubes are composed of the Cnt_Hα and the narrow band filter Hα, which are taken simultaneously to permit the suppression of the speckle pattern. The principal component analysis (PCA) method was employed for the reduction of the data. For each dataset, we derived the 5σ contrast limit and converted it in upper limits on the accretion luminosity. Results. We do not detect any new accreting substellar companions around the targeted transition disks down to an average contrast of 12 magnitudes at 0 . 2 from the central star. We have recovered the signal of the accreting M star companion around the star HD 142527. We have detected and resolved, for the first time in visible light, the quadruple system HD 98800. For every other system, we can exclude the presence of massive actively accreting companions, assuming that the accretion is not episodic and that the extinction is negligible. The mean accretion luminosity limit is 10 −6 L at a separation of 0 . 2 from the host.

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Detection of Hα emission from PZ Telescopii B using SPHERE/ZIMPOL

Cited by 6 publications

References 46 publications

Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*

Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*

Strong Hα emission and signs of accretion in a circumbinary planetary mass companion from MUSE

The widest Hα survey of accreting protoplanets around nearby transition disks

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