Enhanced Data Discovery Services for the ESO Science Archive

Romaniello, M.; Zampieri, Stefano; Delmotte, N.; Forchì, Vincenzo; Hainaut, Olivier; Micol, A.; Retzlaff, J.; Vera, I.; Fourniol, Nathalie; Khan, Mubashir Ahmed; Uwe, Lange; Devendra, Sisodia; Malgorzata, Stellert; Stoehr, F.; Arnaboldi, M.; Spiniello, C.; Mascetti, Laura; Sterzik, M.

doi:10.18727/0722-6691/5073

Cited by 3 publications

(2 citation statements)

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“…For this initial demonstration, we used the publicly available, fully reduced MUSE data cubes (see Romaniello et al 2018) in the ESO Archive to derive PNLFs across a range of galaxy types and distances. We did not sift through the archive completely, but rather, we selected three representative systems that are amenable for analysis and validation of our methodology.…”

Section: Observationsmentioning

confidence: 99%

Towards Precision Cosmology With Improved PNLF Distances Using VLT-MUSE I. Methodology and Tests

Roth,

Jacoby,

Ciardullo

et al. 2021

Preprint

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The [O III] λ5007 Planetary Nebula Luminosity Function (PNLF) is an established distance indicator that has been used for more than 30 years to measure the distances of galaxies out to ∼ 15 Mpc. With the advent of the Multi-Unit Spectroscopic Explorer on the Very Large Telescope (MUSE) as an efficient wide-field integral field spectrograph, the PNLF method is due for a renaissance, as the spatial and spectral information contained in the instrument's datacubes provides many advantages over classical narrow-band imaging. Here we use archival MUSE data to explore the potential of a novel differential emission-line filter (DELF) technique to produce spectrophotometry that is more accurate and more sensitive than other methods. We show that DELF analyses are superior to classical techniques in high surface brightness regions of galaxies and we validate the method both through simulations and via the analysis of data from two early-type galaxies (NGC 1380 and NGC 474) and one late-type spiral (NGC 628). We demonstrate that with adaptive optics support or under excellent seeing conditions, the technique is capable of producing precision ( 0.05 mag) [O III] photometry out to distances of 40 Mpc while providing discrimination between planetary nebulae and other emission-line objects such as H II regions, supernova remnants, and background galaxies. These capabilities enable us to use MUSE to measure precise PNLF distances beyond the reach of Cepheids and the tip of the red giant branch method, and become an additional tool for constraining the local value of the Hubble constant.

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Section: Observationsmentioning

confidence: 99%

Towards Precision Cosmology With Improved PNLF Distances Using VLT-MUSE I. Methodology and Tests

Roth,

Jacoby,

Ciardullo

et al. 2021

Preprint

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“…For our analysis, we extracted publicly available, fully reduced MUSE data cubes of the galaxies listed in Table 1 from the ESO archive (Romaniello et al 2018). These data, which were obtained between 2014 June 25 and 2020 December 5, were taken under a variety of observing conditions, with exposure times ranging between 621 and 9600 s, and seeing (as listed in the archive) between 0 51 and 1 27.…”

Section: Observations and Reductionsmentioning

confidence: 99%

Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data

Jacoby,

Ciardullo,

Roth

et al. 2024

ApJS

Self Cite

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Thanks to the MUSE integral field spectrograph on board the Very Large Telescope (VLT), extragalactic distance measurements with the [O iii] λ5007 planetary nebula luminosity function (PNLF) are now possible out to ∼40 Mpc. Here we analyze the VLT/MUSE data for 20 galaxies from the ESO public archive to identify the systems’ planetary nebulae (PNe) and determine their PNLF distances. Three of the galaxies do not contain enough PNe for a robust measure of the PNLF, and the results for one other system are compromised of the galaxy’s internal extinction. However, we obtain robust PNLF distances for the remaining 16 galaxies, two of which are isolated and beyond 30 Mpc in a relatively unperturbed Hubble flow. From these data, we derive a Hubble constant of 74.2 ± 7.2 (stat) ±3.7 (sys) km s−1 Mpc−1, a value that is very similar to that found from other quality indicators (e.g., Cepheids, the tip of the red giant branch, and surface brightness fluctuations). At present, the uncertainty is dominated by the small number of suitable galaxies in the ESO archive and their less-than-ideal observing conditions and calibrations. Based on our experience with these systems, we identify the observational requirements necessary for the PNLF to yield a competitive value for H 0 that is independent of the Type Ia supernova distance scale.

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Tracing the 107 K warm–hot intergalactic medium with UV absorption lines

Fresco

Péroux

Merloni

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Today, the majority of the cosmic baryons in the Universe are not observed directly, leading to an issue of ”missing baryons” at low redshift. Cosmological hydrodynamical simulations have indicated that a significant portion of them will be converted into the so-called Warm-Hot Intergalactic Medium (WHIM), with gas temperature ranging between 105–107K. While the cooler phase of this gas has been observed using O VI and Ne VIII absorbers at UV wavelengths, the hotter fraction detection relies mostly on observations of O VII and O VIII at X-ray wavelengths. Here, we target the forbidden line of [Fe XXI] λ 1354Å which traces 107K gas at UV wavelengths, using more than one hundred high-spectral resolution (R∼49,000) and high signal to noise VLT/UVES quasar spectra, corresponding to over 600 hrs of VLT time observations. A stack of these at the position of known DLAs lead to a 5-σ limit of log[N([Fe XXI])] <17.4 (EWrest < 22mÅ), three orders of magnitude higher than the expected column density of the WHIM log[N([Fe XXI])] <14.5. This work proposes an alternative to X-ray detected 107K WHIM tracers, by targeting faint lines at UV wavelengths from the ground benefiting from higher instrumental throughput, enhanced spectral resolution, longer exposure times and increased number of targets. The number of quasar spectra required to reach this theoretical column density with future facilities including 4MOST, ELT/HIRES, MSE and the Spectroscopic Telescope appears challenging at present. Probing the missing baryons is essential to constrain the accretion and feedback processes which are fundamental to galaxy formation.

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Enhanced Data Discovery Services for the ESO Science Archive

Cited by 3 publications

References 0 publications

Towards Precision Cosmology With Improved PNLF Distances Using VLT-MUSE I. Methodology and Tests

Towards Precision Cosmology With Improved PNLF Distances Using VLT-MUSE I. Methodology and Tests

Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data

Tracing the 107 K warm–hot intergalactic medium with UV absorption lines

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