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Mission Overview

Clusters in the UV as Engines (CLUES)

 

Primary Investigator:  Angela Adamo

HLSP Authors:  Mattia Sirressi

Released:  2024-08-09

Updated:  2024-08-09

Primary Reference(s):  Sirressi et al. 2022

DOI:  10.17909/2bay-1d16

Citations:  See ADS Metrics

Read Me

Source Data:

 
A figure showing a collection of FUV COS spectra for 20 young star clusters with ages between 1 and 50 Myr, which are hosted by nearby star forming galaxies.
Atlas of the CLUES FUV spectra at 0.4 Å spectral resolution, sorted by star cluster age. The vertical dashed lines indicate some of the photospheric lines, stellar wind P-Cygni lines, and absorption lines due to the ISM along the line of sight. These lines are labeled on top of the figure. The regions of the spectra that are not included in the team's analysis such as the Lyα emission, the O I geocoronal line, and the detector gaps at about 1300 Å and 1600 Å are omitted for clarity.

Overview

CLUES is an HST medium-size program (ID 15627, PI: Adamo) that provides FUV spectroscopy of 20 young star clusters in local galaxies (less than 16 Mpc away). Three sources (NGC4449-YSC1, NGC5253-YSC1 and NGC5253-YSC2) were observed as part of an earlier program (ID 11579, PI: Aloisi).

All the CLUES star clusters are very young (<50 Myr) and massive (> 104 Msun) and they are hosted in galaxies that are part of the Hubble treasury program Legacy ExtraGalactic Uv Survey (LEGUS, Calzetti 2015). The team has selected in most cases two clusters per galaxy, at various distances from the center of the galaxy (from 0.1 to 2.8 half-mass radii). The main goals of this project are: (1) derive the stellar population properties of young clusters using FUV spectroscopy, including a measurement of the feedback from stellar winds and supernovae; (2) measure the kinematics of the outflowing gas by modeling the ISM absorption lines in the FUV and connect this to the stellar feedback injected by individual young star clusters.

Data Products

Data file naming convention:

hlsp_clues_hst_cos_<target>_<filter>_v1.0_spectrum-<exten>.fits

where:

  • <target> is the name of the cluster (e.g. "m-74-ysc1")
  • <filter> is one of:
    • "g130m" = grating G130M
    • "g160m" = grating G160M
    • "g130m-g160m" = combination of gratings G130M and G160M

Data file types:

_spectrum.fits FUV observed spectra
-lya.fits Ly-alpha Voigt models
-pop.fits FUV observed spectra (corrected), the stellar population model and the fitting mask
-contnorm.fits FUV observed spectra normalized by the stellar continuum

 

All FITS files are in the BINTABLE format.

Data Access

CLUES spectra are available in the MAST Portal (web-based, cross-mission search interface) and Astroquery (Python package to search for and download files from Python scripts you write). Set the Provenance Name filter to CLUES in the Portal Advanced Search to find all or individual spectra.

from astroquery.mast import Observations
all_obs = Observations.query_criteria(provenance_name="clues")
data_products = Observations.get_product_list(all_obs)
Observations.download_products(data_products)

  • MAST Portal

    Link to the MAST Portal Webpage
    A web-based interface for cross-mission searches of data at MAST or the Virtual Observatory
    Portal

  • MAST Astroquery

    MAST Astroquery
    Search for and retrieve CLUES data products programmatically.
    MAST Astroquery

Citations

Please remember to cite the appropriate paper(s) below and the DOI if you use these data in a published work. 

Note: These HLSP data products are licensed for use under CC BY 4.0.

References

Sirressi et al. 2022

CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light

Sirressi et al. 2024

CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback