The Japanese space gravitational wave antenna: DECIGO

By S. Kawamura, M. Ando, N. Seto, S. Sato, Takashi Nakamura, K. Tsubono, N. Kanda, Takahiro Tanaka, J. Yokoyama, I. Funaki and 134 more. 2011

504 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7ef209b07162a047ad9553605228ffb814f9ea82

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Paolo Pani
2. R. Brito
3. V. Cardoso
4. Marek Lewicki
5. John Ellis
6. J. No
7. V. Vaskonen
8. R. Cai

Citations in the corpus

• Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic N-body Dynamics (2018, background): “The 3-body mergers (red) all have a much higher initial fGW with a peak between 10 0 − 101 Hz, and will therefore elude the LISA band and form directly in the proposed DECIGO (Kawamura et al. 2011; Isoyama et al. 2018)/Tian Qin (Luo et al. 2016) band before entering the LIGO band (e.g., Chen & Amaro”
• Gravitational wave energy budget in strongly supercooled phase transitions (2019, methodology): “). Incidentally, this strongly enhances the interest of possible experiments sensitive to frequencies between 10 2 and 1Hz, such as MAGIS [72] and the similar AION proposal [73] as well as the DECIGO [76] and BBO [77,78] proposals. Acknowledgments The work of JE, ML and VV was supported by the UK ST”
• Primordial black holes and gravitational waves from parametric amplification of curvature perturbations (2019, methodology): “We compare them with the constrain or the sensitivity curves of GW detectors including EPTA [100], NANOGrav [101], PPTA [102], SKA [103], LISA [104], Taiji [105], DECIGO [106], BBO [107], KAGRA [108], aLIGO [109], ET [110].”
• Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “sitivity is limited mainly by the seismic noises at such lower frequencies. However these signals may be detectable by the recently proposed future space interferometers like Fabry-Perot type DECIGO ([148], black line in the bottom panel). Contributed by the neutrino GWs in the lower frequency domai”
• On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, result): “tivities of LISA [93], the Einstein Telescope (ET) [94,95], the Cosmic Explorer (CE) [96], and the Square Kilometre Array (SKA) [97]. Finally, we also show the prospective sensitivities of the DECIGO [98] and Big Bang Observer (BBO) [99,100] projects in the frequency range between LISA and LIGO (ano”
• Superradiance (2015, methodology): “With the addition of a detector in the deci-Hz such as the proposed DECIGO [653], bosons with masses in the range 10−19 eV .”