<i>PlanetCam UPV/EHU</i>: A Two-channel Lucky Imaging Camera for Solar System Studies in the Spectral Range 0.38–1.7<i>μ</i>m

Mendikoa, I.; Sánchez‐Lavega, A.; Pérez‐Hoyos, S.; Hueso, R.; Rojas, J. F.; Aceituno, J.; Aceituno, F. J.; Murga, Gaizka; Bilbao, L. de; García-Melendo, E.

doi:10.1088/1538-3873/128/961/035002

Cited by 26 publications

(44 citation statements)

References 53 publications

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“…However, this also depends on the filter, with resolutions better that 0.5" for wide filters used for lucky-imaging and overall better behavior in the SWIR channel (Mendikoa et al 2016).…”

Section: Resultsmentioning

confidence: 99%

“…This consists of the acquisition in a short time of several hundredths to thousands of short exposures (10s of milliseconds) selected by their quality and stacked into a single image (Law et al 2006) for broadband filters, and longer exposures (i.e., a few seconds each and also stacked for building high signal-to-noise ratio images) for narrowband imaging. The final stacked images are processed to obtain high-resolution 1 https://archive.stsci.edu/prepds/opal/ observations that largely remove the blur from atmospheric effects (Mendikoa et al 2016). The selection of the best 1-10% of frames without adding any additional image processing results in high-quality images that retain the photometry of the object observed.…”

Section: Planetcam Instrumentmentioning

confidence: 99%

“…Table 1 provides details on these campaigns, including the telescope and PlanetCam configuration (Mendikoa et al 2016). The PlanetCam1 (PC1) configuration means that only the visible channel (VIS) was available at the time, while PlanetCam2 (PC2) means that both the visible and infrared (SWIR) channels were available.…”

Section: Observation Campaignsmentioning

confidence: 99%

“…These images preserve photometric information but can be high-pass filtered to show faint struc- tures and study dynamics (see, e.g., Hueso et al 2017b). All the PlanetCam filters are listed by their short name and we provide below effective wavelength in nanometers for narrow filters (full details can be found in Mendikoa et al 2016). The VIS channel includes filters U, Vio, B, V, R, M1 (619) …”

Section: Image Acquisition and Processingmentioning

confidence: 99%

“…Filters JM and V3 are not included in Fig. 7 because they are affected by telluric water absorption, while the HM filter is affected by the cutoff of the sensitivity of the PlanetCam SWIR detector (Mendikoa et al, 2016). The number of campaigns considered and average uncertainties for these filters are as follows: YC (four; 24%), YM (four; 19%), V1 (four; 12%), V2 (three; 22%), JC (four; 18%), and HC (four; 11%).…”

Section: Absolute Reflectivity Valuesmentioning

confidence: 99%

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Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

Mendikoa¹,

Sánchez‐Lavega²,

Pérez‐Hoyos³

et al. 2017

A&A

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Aims. We provide measurements of the absolute reflectivity of Jupiter and Saturn along their central meridians in filters covering a wide range of visible and near-infrared wavelengths (from 0.38 to 1.7 µm) that are not often presented in the literature. We also give measurements of the geometric albedo of both planets and discuss the limb-darkening behavior and temporal variability of their reflectivity values for a period of four years (2012)(2013)(2014)(2015)(2016).Methods. This work is based on observations with the PlanetCam-UPV/EHU instrument at the 1.23 m and 2.2 m telescopes in Calar Alto Observatory (Spain). The instrument simultaneously observes in two channels: visible (VIS; 0.38-1.0 µm) and short-wave infrared (SWIR; 1.0-1.7 µm). We obtained high-resolution observations via the lucky-imaging method. Results. We show that our calibration is consistent with previous independent determinations of reflectivity values of these planets and, for future reference, provide new data extended in the wavelength range and in the time. Our results have an uncertainty in absolute calibration of 10-20%. We show that under the hypothesis of constant geometric albedo, we are able to detect absolute reflectivity changes related to planetary temporal evolution of about 5-10%.

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“…However, this also depends on the filter, with resolutions better that 0.5" for wide filters used for lucky-imaging and overall better behavior in the SWIR channel (Mendikoa et al 2016).…”

Section: Resultsmentioning

confidence: 99%

Section: Planetcam Instrumentmentioning

confidence: 99%

Section: Observation Campaignsmentioning

confidence: 99%

Section: Image Acquisition and Processingmentioning

confidence: 99%

Section: Absolute Reflectivity Valuesmentioning

confidence: 99%

See 3 more Smart Citations

Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

Mendikoa¹,

Sánchez‐Lavega²,

Pérez‐Hoyos³

et al. 2017

A&A

View full text Add to dashboard Cite

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A planetary‐scale disturbance in the most intense Jovian atmospheric jet from JunoCam and ground‐based observations

Sánchez‐Lavega

Rogers

Orton

et al. 2017

Geophysical Research Letters

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We describe a huge planetary‐scale disturbance in the highest‐speed Jovian jet at latitude 23.5°N that was first observed in October 2016 during the Juno perijove‐2 approach. An extraordinary outburst of four plumes was involved in the disturbance development. They were located in the range of planetographic latitudes from 22.2° to 23.0°N and moved faster than the jet peak with eastward velocities in the range 155 to 175 m s−1. In the wake of the plumes, a turbulent pattern of bright and dark spots (wave number 20–25) formed and progressed during October and November on both sides of the jet, moving with speeds in the range 100–125 m s−1 and leading to a new reddish and homogeneous belt when activity ceased in late November. Nonlinear numerical models reproduce the disturbance cloud patterns as a result of the interaction between local sources (the plumes) and the zonal eastward jet.

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Jupiter cloud morphology and zonal winds from ground‐based observations before and during Juno's first perijove

Hueso

Sánchez‐Lavega

Iñurrigarro

et al. 2017

Geophysical Research Letters

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We analyze Jupiter observations between December 2015 and August 2016 in the 0.38–1.7 μm wavelength range from the PlanetCam instrument at the 2.2 m telescope at Calar Alto Observatory and in the optical range by amateur observers contributing to the Planetary Virtual Observatory Laboratory. Over this time Jupiter was in a quiescent state without notable disturbances. Analysis of ground‐based images and Hubble Space Telescope observations in February 2016 allowed the retrieval of mean zonal winds from −74.5° to +73.2°. These winds did not change over 2016 or when compared with winds from previous years with the sole exception of intense zonal winds at the North Temperate Belt. We also present results concerning the major wave systems in the North Equatorial Belt and in the upper polar hazes visible in methane absorption bands, a description of the planet's overall cloud morphology and observations of Jupiter hours before Juno's orbit insertion.

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PlanetCam UPV/EHU: A Two-channel Lucky Imaging Camera for Solar System Studies in the Spectral Range 0.38–1.7μm

Cited by 26 publications

References 53 publications

Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

A planetary‐scale disturbance in the most intense Jovian atmospheric jet from JunoCam and ground‐based observations

Jupiter cloud morphology and zonal winds from ground‐based observations before and during Juno's first perijove

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