This Hubble image features four of the thousands of galaxies found within the Hubble Ultra Deep Field. All of the highlighted galaxies show evidence of vigorous star formation (blue regions filled with hot, young stars). In the insets at right, the near-infrared spectrum of each galaxy is displayed. By examining a galaxy’s spectrum, you can learn about the ages of its stars, its star-formation history, how many heavy chemical elements it contains, and more.
Upon entering operations in 2027, the Nancy Grace Roman Space Telescope will be able to collect spectra for every object in its field of view, which is 200 times larger than Hubble’s in infrared light. As a result, it will enable studies of rare galaxies from a period known as “cosmic noon,” when many galaxies went through growth spurts.
Credits
Science
NASA, ESA, STScI, Casey Papovich (TAMU)
Image Processing
Alyssa Pagan (STScI)
| About The Object | |
|---|---|
| Object Name | HLF; GS3-40891; GS4-30760; GS4-29845; GS4-29048 |
| Object Description | Deep field with spectra of starburst galaxies |
| R.A. Position | 3:32:29 |
| Dec. Position | -27:49:12 |
| Constellation | Fornax |
| About The Data | |
| Data Description | Image: The HLF image was created from public archive Hubble data from the following proposals: , , , , and : A. Riess (STScI/JHU); : M. Giavalsco (University of Massachusetts); , and : J. Rhodes (JPL); : K. Ratnatunga (Carnegie Mellon University); : H. Rix (MPE) : W. Sparks (STScI); , , and : S. Malhotra (Arizona State University); : R. Thompson (University of Arizona) and : S. Beckwith (STScI); : C. Kretchmer (JHU); : M. Stiavelli (STScI); R. Bouwens (Universiteit Leiden); : R. O'Connell (University of Virginia); , and 12007: G. Illingworth (University of California, Santa Cruz); , , and : S. Faber (University of California, Santa Cruz); : P. van Dokkum (Yale University). : R. Ellis (University College London) : H. Teplitz (California Institute of Technology) : M. Swinbank (Durham University) : A. Muzzin (York University) : P. Oesch (Observatoire de Geneve) : E. Vanzella (INAF) The HLF team members include: G. Illingworth and D. Magee (University of California, Santa Cruz), K. Whitaker (University of Connecticut), R. Bouwens (Leiden University), P. Oesch (University of Geneva), P. van Dokkum (Yale University), I. Labbe (Swinburne University), B. Holden (University of California, Santa Cruz), M. Franx (Leiden University), and V. Gonzalez (Universidad de Chile). Spectra: The Hubble image(spectra) was created from HST data from proposal: (C. Papovich). |
| Instrument | ACS/WFC, WFC3/IR, WFC3/UVIS |
| Filters | WFC3/UV (F225W, F275W, and F336W); ACS (F435W, F606W, F775W, F814W, and F850LP); WFC3/IR (G102, F098M, F105W, F125W, F140W, and F160W) |
| About The Image | |
| Color Info | IMAGE: These images are composites of separate exposures acquired by the ACS and WFC3 instruments on the Hubble Space Telescope. Several filters were used to sample broad and narrow wavelength ranges. The color results from assigning different hues (colors) to each monochromatic (grayscale) image associated with an individual filter. In this case, the assigned colors are: Blue: F606W (Wide V) Green: F606W (Wide V) and F850LP (SDSS z') Red: F850LP (SDSS z') SPECTRA: The spectra is created from exposures from the WFC3/IR instrument using a grism. A color map from yellow to red is applied to the spectra which corresponds to increasing wavelength. |
| About The Object | |
|---|---|
| Object Name | A name or catalog number that astronomers use to identify an astronomical object. |
| Object Description | The type of astronomical object. |
| R.A. Position | Right ascension – analogous to longitude – is one component of an object's position. |
| Dec. Position | Declination – analogous to latitude – is one component of an object's position. |
| Constellation | One of 88 recognized regions of the celestial sphere in which the object appears. |
| Distance | The physical distance from Earth to the astronomical object. Distances within our solar system are usually measured in Astronomical Units (AU). Distances between stars are usually measured in light-years. Interstellar distances can also be measured in parsecs. |
| Dimensions | The physical size of the object or the apparent angle it subtends on the sky. |
| About The Data | |
| Data Description |
|
| Instrument | The science instrument used to produce the data. |
| Exposure Dates | The date(s) that the telescope made its observations and the total exposure time. |
| Filters | The camera filters that were used in the science observations. |
| About The Image | |
| Image Credit | The primary individuals and institutions responsible for the content. |
| Publication Date | The date and time the release content became public. |
| Color Info | A brief description of the methods used to convert telescope data into the color image being presented. |
| Orientation | The rotation of the image on the sky with respect to the north pole of the celestial sphere. |
